Дисертації: "Formation and evolution of planetary systems"

1

Inamdar, Niraj K. "The formation and evolution of planetary systems." Thesis, Massachusetts Institute of Technology, 2016. http://hdl.handle.net/1721.1/107104.

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Thesis: Ph. D. in Planetary Science, Massachusetts Institute of Technology, Department of Earth, Atmospheric, and Planetary Sciences, 2016. Cataloged from PDF version of thesis. Includes bibliographical references (pages 299-311). The Kepler space observatory and other surveys have revealed thousands of planets and planetary systems that look significantly different from our own. In particular, the preponderance of super-Earths and mini-Neptunes (planets with radii smaller than Neptune's but larger than Earth's) at short orbital radii has challenged planet formation theories developed in the context of our own Solar System. How and where these planets form remains an outstanding question. Given the large frequency with which such planets occur around other stars, understanding the formation pathways of these planets has the potential to reveal dominant mechanisms for planet formation and evolution and to place our own Solar System within a broader context. The purpose of this thesis is to address and develop frameworks by which these questions can be answered. The thesis is comprised of two parts. In Part I, we consider the question of how and where close-in exoplanets formed. We do this in two ways. First, we use that fact that many close-in super-Earths and mini-Neptunes possess gaseous envelopes that comprise several percent or more of the total planet mass in order to construct a self-consistent planet formation history that accounts for core accretion, thermal evolution, and dynamical interactions during the core assembly process via giant impacts. We find that envelope masses accreted from the gas disc by planetary embryos are typically much smaller than those inferred for many exoplanets, and that the envelope mass fraction is further reduced substantially during the assembly phase when embryos merge. Fully assembled planets can accrete observed envelope masses from the residual disc only if energy exchange between the envelope and the underlying core is totally inhibited. It is therefore very unlikely that such planets formed at their observed semimajor axes, but instead formed further out and migrated inwards. Second, we consider the late-stage evolution of exoplanets after gas disc dissipation in order to explain the bulk structural diversity of observed super-Earths and mini-Neptunes. Whereas naive application of core accretion models suggests a narrow mass-radius relationship for these exoplanets, the population possesses a great deal of diversity in mean density. While photoevaporative mass loss from the host star is the most-commonly invoked explanation for this diversity, we use the fact that many exoplanetary systems are in tightly packed orbital configurations to propose instead that late-stage collisions are at least in part responsible for the observed diversity. We infer envelope mass fractions for planets in the literature whose masses and radii have been measured, and on the basis of this, we identify multiplanet systems whose bulk structural diversity favors late-stage impacts as opposed to photoevaporative devolatilization. In Part II, we turn our attention to the formation and evolution of our own Solar System. We do this within the context of NASA's OSIRIS-REx asteroid sample return mission. OSIRIS-REx, which launches in September 2016, will arrive at the near-Earth asteroid 101955 Bennu in 2019 with the objective of constraining its composition, orbit, and other bulk properties. In order to better understand the composition of Bennu, an instrument designed to measure its elemental abundances via X-ray fluorescence spectroscopy called REXIS was developed and built at MIT. In this part of the thesis, we investigate the ability of REXIS to constrain the composition of Bennu via fluorescence spectroscopy, as well as its potential to place Bennu within an analogue meteorite class. We carry out our analysis by modeling Solar X-ray activity and the X-ray fluorescence from Bennu, as well as by simulating data product and analysis from the instrument in order to predict REXIS's ability to carry out its goal of contextualizing Bennu within the asteroid and meteorite population. by Niraj K. Inamdar. Ph. D. in Planetary Science

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2

Payne, Matthew John. "On the formation and evolution of planetary systems." Thesis, University of Cambridge, 2009. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.611755.

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3

Hands, Thomas Oliver. "The enthralling tale of the formation and evolution of compact planetary systems." Thesis, University of Leicester, 2016. http://hdl.handle.net/2381/38766.

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Of the myriad of insights into exoplanetary systems provided by the Kepler mission, one of the most intriguing new discoveries is that of a class of compact planetary systems which include Kepler-11, Kepler-32 and Kepler-90. In such systems, ensembles of several planets are found in very closely packed orbits (often within a few percent of an astronomical unit of one another). These systems present a challenge for traditional formation and migration scenarios, since these planets presumably formed at larger orbital radii before migrating inwards. In particular, it is difficult to understand how some planets in such systems could have migrated across strong mean-motion resonances without becoming trapped, and remaining relatively well-spaced. It is also difficult to explain how such systems remain dynamically cold, as resonant interactions tend to excite orbital eccentricity and lead to close encounters. I present a dynamical study of the formation of these systems, using an N-body method which incorporates a parametrized model of planet migration in a turbulent protoplanetary disc. The study explores a wide parameter space, and finds that under suitable conditions it is possible to form compact, close-packed planetary systems via traditional disc-driven migration, albeit with an over-abundance of mean-motion resonances. I then extend the study to include Jupiter-mass planets exterior to the compact systems, and find that the dynamical effect of these companions can significantly modify the resonant structure of the compact planets. Finally, I extend this work to two dimensional hydrodynamical simulations in an attempt to model type I migration self-consistently. In particular, I find that clearing of the disc by photoevaporation can halt migration of compact systems, and also discover that planet-disc interactions can - under the right conditions - break mean-motion resonances.

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4

Davies, Claire L. "Revolution evolution : tracing angular momentum during star and planetary system formation." Thesis, University of St Andrews, 2015. http://hdl.handle.net/10023/7557.

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Stars form via the gravitational collapse of molecular clouds during which time the protostellar object contracts by over seven orders of magnitude. If all the angular momentum present in the natal cloud was conserved during collapse, stars would approach rotational velocities rapid enough to tear themselves apart within just a few Myr. In contrast to this, observations of pre-main sequence rotation rates are relatively slow (∼ 1 − 15 days) indicating that significant quantities of angular momentum must be removed from the star. I use observations of fully convective pre-main sequence stars in two well-studied, nearby regions of star formation (namely the Orion Nebula Cluster and Taurus-Auriga) to determine the removal rate of stellar angular momentum. I find the accretion disc-hosting stars to be rotating at a slower rate and contain less specific angular momentum than the disc-less stars. I interpret this as indicating a period of accretion disc-regulated angular momentum evolution followed by near-constant rotational evolution following disc dispersal. Furthermore, assuming that the age spread inferred from the Hertzsprung-Russell diagram constructed for the star forming region is real, I find that the removal rate of angular momentum during the accretion-disc hosting phase to be more rapid than that expected from simple disc-locking theory whereby contraction occurs at a fixed rotation period. This indicates a more efficient process of angular momentum removal must operate, most likely in the form of an accretion-driven stellar wind or outflow emanating from the star-disc interaction. The initial circumstellar envelope that surrounds a protostellar object during the earliest stages of star formation is rotationally flattened into a disc as the star contracts. An effective viscosity, present within the disc, enables the disc to evolve: mass accretes inwards through the disc and onto the star while momentum migrates outwards, forcing the outer regions of the disc to expand. I used spatially resolved submillimetre detections of the dust and gas components of protoplanetary discs, gathered from the literature, to measure the radial extent of discs around low-mass pre-main sequence stars of ∼ 1−10 Myr and probe their viscous evolution. I find no clear observational evidence for the radial expansion of the dust component. However, I find tentative evidence for the expansion ofthe gas component. This suggests that the evolution of the gas and dust components of protoplanetary discs are likely governed by different astrophysical processes. Observations of jets and outflows emanating from protostars and pre-main sequence stars highlight that it may also be possible to remove angular momentum from the circumstellar material. Using the sample of spatially resolved protoplanetary discs, I find no evidence for angular momentum removal during disc evolution. I also use the spatially resolved debris discs from the Submillimetre Common-User Bolometer Array-2 Observations of Nearby Stars survey to constrain the amount of angular momentum retained within planetary systems. This sample is compared to the protoplanetary disc angular momenta and to the angular momentum contained within pre-stellar cores. I find that significant quantities of angular momentum must be removed during disc formation and disc dispersal. This likely occurs via magnetic braking during the formation of the disc, via the launching of a disc or photo-evaporative wind, and/or via ejection of planetary material following dynamical interactions.

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5

Meng, Huan Y. A., George H. Rieke, Kate Y. L. Su, and András Gáspár. "The First 40 Million Years of Circumstellar Disk Evolution: The Signature of Terrestrial Planet Formation." IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/623246.

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We characterize the first 40 Myr of evolution of circumstellar disks through a unified study of the infrared properties of members of young clusters and associations with ages from 2 Myr up to similar to 40 Myr: NGC 1333, NGC 1960, NGC 2232, NGC 2244, NGC 2362, NGC 2547, IC 348, IC 2395, IC 4665, Chamaeleon I, Orion OB1a and OB1b, Taurus, the beta Pictoris Moving Group,. Ophiuchi, and the associations of Argus, Carina, Columba, Scorpius-Centaurus, and Tucana-Horologium. Our work features: (1) a filtering technique to flag noisy backgrounds; (2) a method based on the probability distribution of deflections, P(D), to obtain statistically valid photometry for faint sources; and (3) use of the evolutionary trend of transitional disks to constrain the overall behavior of bright disks. We find that the fraction of disks three or more times brighter than the stellar photospheres at 24 mu m decays relatively slowly initially and then much more rapidly by similar to 10 Myr. However, there is a continuing component until similar to 35 Myr, probably due primarily to massive clouds of debris generated in giant impacts during the oligarchic/chaotic growth phases of terrestrial planets. If the contribution from primordial disks is excluded, the evolution of the incidence of these oligarchic/chaotic debris disks can be described empirically by a log-normal function with the peak at 12-20 Myr, including similar to 13% of the original population, and with a post-peak mean duration of 10-20 Myr.

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6

Trilling, David Eric. "A theoretical and observational study of the formation and evolution of planetary systems and extrasolar planets." Diss., The University of Arizona, 1999. http://hdl.handle.net/10150/288998.

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The recent discoveries of extrasolar giant planets (planets like Jupiter orbiting other stars like our Sun) at small distances from their central stars have revitalized the fields of planet and planetary system formation. The discoveries have overturned the former paradigm for planetary system formation which suggested that all planetary systems would look like our Solar System: these decidedly do not. The new view is that the early solar system was not nearly the quiescent place previously thought, but rather a dynamic environment in which planets are both easily created and easily destroyed. I have participated in the building of a new paradigm of planetary system formation, and this thesis describes theoretical and observational work which have contributed to this field. My theoretical work on the migration of giant planets from their formation location to distances close to their central star is described. I show that giant planets can reside at a range of heliocentric distances and masses, and we reproduce the distribution of observed giant planets, as well Jupiter. Using this model, I have predicted what the rate of planet formation must be, and what the initial, mass function for forming planets must be, in order to reproduce the observed planets. I also place some constraints on the mass and viscosity of the circumstellar disk out of which planets form. I show that giant planets close to their central stars are tidally stable, and stable against atmospheric loss, contrary to intuition. I predict that tidally stripped rocky cores, the remnants of giant planets, should exist at small heliocentric distances, a byproduct of the migration and mass loss that a majority of giant planets go through. Lastly, as an outgrowth of our migration work, I designed an observing program to search for circumstellar disks around stars with known extrasolar planets. I have detected three such disks, analogs to our Solar System's Kuiper Belt, and failed to detect disks around three other stars with extrasolar planets. I discuss my observing results, and the implications of detecting disks around some, but not all, of the stars with extrasolar planets I have looked at. In the conclusions and future work, I describe how this work forms a coherent part of a larger goal of understanding how, where, and how often planets and planetary systems form, answering the question of the origin, nature, and uniqueness of our Solar System.

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7

Ngo, Henry, Heather A. Knutson, Sasha Hinkley, et al. "FRIENDS OF HOT JUPITERS. IV. STELLAR COMPANIONS BEYOND 50 au MIGHT FACILITATE GIANT PLANET FORMATION, BUT MOST ARE UNLIKELY TO CAUSE KOZAI–LIDOV MIGRATION." IOP PUBLISHING LTD, 2016. http://hdl.handle.net/10150/621385.

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Stellar companions can influence the formation and evolution of planetary systems, but there are currently few observational constraints on the properties of planet-hosting binary star systems. We search for stellar companions around 77 transiting hot Jupiter systems to explore the statistical properties of this population of companions as compared to field stars of similar spectral type. After correcting for survey incompleteness, we find that 47% +/- 7% of hot Jupiter systems have stellar companions with semimajor axes between 50 and 2000 au. This is 2.9 times larger than the field star companion fraction in this separation range, with a significance of 4.4 sigma. In the 1-50 au range, only 3.9(-2.0)(+4.5)% of hot Jupiters host stellar companions, compared to the field star value of 16.4% +/- 0.7%, which is a 2.7 sigma difference. We find that the distribution of mass ratios for stellar companions to hot Jupiter systems peaks at small values and therefore differs from that of field star binaries which tend to be uniformly distributed across all mass ratios. We conclude that either wide separation stellar binaries are more favorable sites for gas giant planet formation at all separations, or that the presence of stellar companions preferentially causes the inward migration of gas giant planets that formed farther out in the disk via dynamical processes such as Kozai-Lidov oscillations. We determine that less than 20% of hot Jupiters have stellar companions capable of inducing Kozai-Lidov oscillations assuming initial semimajor axes between 1 and 5 au, implying that the enhanced companion occurrence is likely correlated with environments where gas giants can form efficiently.

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8

Philipot, Florian. "Vers une recherche exhaustive des planètes géantes autour des étoiles proches de type solaire." Electronic Thesis or Diss., Université Paris sciences et lettres, 2023. http://www.theses.fr/2023UPSLO008.

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La détection des premières exoplanètes dans les années 1990 a ouvert une nouvelle ère dans l'étude des planètes. Aujourd'hui, grâce aux instruments toujours plus performants, plusieurs centaines d'exoplanètes (Jupiters chauds, Super-Terre, systèmes multiples...) sont découvertes chaque année. Grâce à cette grande variété d'exoplanètes, il est possible d'étudier la distribution (distance, masse, excentricité...) de ces objets afin de mieux contraindre les modèles de formation et d'évolution des systèmes planétaires. Néanmoins, chaque méthode de détection a ses limites et ses biais de détection. Un des objectifs de cette thèse fut de mettre en évidence les limites des différentes méthodes de détection, en particulier celles liées aux vitesses radiales (VR), et d'améliorer la caractérisation des compagnons détectés en VR.Dans un premier temps, j'ai testé la solidité des études visant à déterminer la distribution radiale des planètes géantes. L'analyse des données de VR des étoiles abritant des planètes à longues périodes, de l'impact de l'activité stellaire et des hypothèses faites lors des calculs d'exhaustivité, nous a permis de démontrer que les études statistiques en VR n'étaient pas robustes au-delà de 7-8 ua. Par la suite, j'ai combiné des données de VR avec les mesures d'astrométrie absolue et relative disponibles dans le but d'améliorer la caractérisation des compagnons sub-stellaires à longues périodes. Cette étude a permis de contraindre précisément les paramètres orbitaux et, surtout, la masse de sept compagnons détectés en VR. Elle a également permis de mettre en avant l'importance du couplage des données de VR avec d'autres mesures afin de déterminer avec précision la nature d'un compagnon. Pour finir, j'ai utilisé les mesures d'anomalie de mouvements propres (PMa) des étoiles, estimées à partir des mesures astrométriques des télescopes Hipparcos et Gaia, dans le but de rechercher de nouveaux compagnons sub-stellaires dans les archives du spectrographe HARPS/VLT. Cette analyse m'a permis d'améliorer la caractérisation de 14 compagnons sub-stellaires et de découvrir trois nouvelles naines brunes ainsi que sept nouvelles exoplanètes. J'ai également pu démontrer l'efficacité de l'utilisation des mesures de PMa pour optimiser la recherche de compagnons sub-stellaires The detection of the first exoplanets in the 1990s opened a new era in the study of planets. Today, thanks to increasingly powerful instruments, several hundred exoplanets (hot Jupiters, Super-Earths, multiple systems...) are discovered every year. Thanks to this wide variety of exoplanets, it is possible to study the distribution (distance, mass, eccentricity...) of these objects in order to better constrain the formation and evolution models of planetary system. Nevertheless, each detection method has its own limitations and detection biases. One aim of this thesis was to identify the limitations of the various detection methods, in particular those related to radial velocities (RV), and to improve the characterization of companions detected by RV.As a first step, I tested the robustness of studies aimed at determining the radial distribution of giant planets. Analysis of RV data from stars hosting long-period planets, the impact of stellar activity and the hypothesis made in completeness calculations, allowed us to demonstrate that statistical RV studies were not robust beyond 7-8 AU. Subsequently, I combined RV data with available absolute and relative astrometry measurements to improve the characterization of long-period sub-stellar companions. This study allowed us to precisely constrain the orbital parameters and, above all, the mass of seven companions detected in RV. It also highlighted the importance of coupling RV data with other measurements to accurately determine the nature of a companion. Finally, I used measurements of stars' proper motion anomalies (PMa), derived from Hipparcos and Gaia absolute astrometry, to search for new sub-stellar companions in the HARPS/VLT spectrograph archive. This analysis enabled me to improve the characterization of 14 sub-stellar companions, and to discover three new brown dwarfs and seven new exoplanets. I also demonstrated the effectiveness of using PMa measurements to optimize the search for sub-stellar companions

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9

Tabera, Martin Luis. "Evolution and properties of planetary systems." Thesis, Uppsala universitet, Observationell astrofysik, 2020. http://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-438128.

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10

Bonsor, Amy Hannah Clay. "Post-main sequence evolution of planetary systems." Thesis, University of Cambridge, 2011. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.609856.

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11

Parai, Rita. "Volatiles in the Earth and Moon: Constraints on planetary formation and evolution." Thesis, Harvard University, 2014. http://dissertations.umi.com/gsas.harvard:11652.

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The volatile inventories of the Earth and Moon reflect unique histories of volatile acquisition and loss in the early Solar System. The terrestrial volatile inventory was established after the giant impact phase of accretion, and the planet subsequently settled into a regime of long-term volatile exchange between the mantle and surface reservoirs in association with plate tectonics. Therefore, volatiles in the Earth and Moon shed light on a diverse array of processes that shaped planetary bodies in the Solar System as they evolved to their present-day states. Earth and Planetary Sciences

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12

McCormick, David S. "Evolution of an early proterozoic alluvially-dominated foreland basis, Burnside Formation, Kilohigok Basin, N.W.T., Canada." Thesis, Massachusetts Institute of Technology, 1992. http://hdl.handle.net/1721.1/31033.

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Thesis (Ph. D.)--Massachusetts Institute of Technology, Dept. of Earth, Atmospheric, and Planetary Sciences, 1992. Vita. Includes bibliographical references. by David Speir McCormick. Ph.D.

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13

Comito, Carlo. "Numerical N-body approach to binary asteroid formation and evolution." Phd thesis, Université de Nice Sophia-Antipolis, 2012. http://tel.archives-ouvertes.fr/tel-00703696.

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Les astéroïdes binaires ont un rôle d'importance fondamentale dans la détermination de paramètres astéroïdales difficilement mesurables de la Terre, en particulier la masse. En étudiant l'origine des binaires dans le cadre des agrégats gravitationnels, ils servent ainsi comme laboratoires naturels pour la physique des systèmes granulaires à basse gravité, et ils nous donnent des éléments précieux pour la modélisation globale des astéroïdes. Vue la grande diversité existante de caractéristiques des systèmes binaires observés, nombreuses hypothèses ont été postulées pour leur origine (fragmentation catastrophique d'un corps et ré-accumulation sous forme binaire, influences de marée par les planètes, cratérisation, YORP ...). Dans cette thèse nous explorons, grâce à des simulations numériques à N corps, la dynamique d'un agrégat gravitationnel en dehors du régime de stabilité pour un corps simple, en cherchant les configurations les plus favorables à la formation d'un système binaire. Dans une première partie, nous montrons que dans un scénario catastrophique la formation de systèmes binaires est normale, ces-ci bien reproduisant la variété présente dans la population observée. En suite, nous explorons la possibilité d'une déformation progressive d'un agrégat vers un système binaire sous l'action d'une force perturbante agissant lentement jusqu'à la fission éventuelle du corps. Nos résultats proposent des nouveaux regards dans l'étude de la formation des astéroïdes binaires, comme montré par une comparaison avec les observations et la littérature existante.

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14

Gerškevitš, Jelena. "Formation and evolution of binary systems with compact objects /." Tartu : Tartu Univ. Press, 2002. http://www.gbv.de/dms/goettingen/389917176.pdf.

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15

Rein, Hanno. "The effects of stochastic forces on the evolution of planetary systems and Saturn's rings." Thesis, University of Cambridge, 2010. https://www.repository.cam.ac.uk/handle/1810/237379.

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The increasing number of discovered extra-solar planets opens a new opportunity for studies of the formation of planetary systems. Their diversity keeps challenging the long-standing theories which were based on data primarily from our own solar system. Resonant planetary systems are of particular interest because their dynamical configuration provides constraints on the otherwise unobservable formation and migration phase. In this thesis, formation scenarios for the planetary systems HD128311 and HD45364 are presented. N-body simulations of two planets and two dimensional hydrodynamical simulations of proto-planetary discs are used to realistically model the convergent migration phase and the capture into resonance. The results indicate that the proto-planetary disc initially has a larger surface density than previously thought. Proto-planets are exposed to stochastic forces, generated by density fluctuations in a turbulent disc. A generic model of both a single planet, and two planets in mean motion resonance, being stochastically forced is presented and applied to the system GJ876. It turns out that GJ876 is stable for reasonable strengths of the stochastic forces, but systems with lighter planets can get disrupted. Even if a resonance is not completely disrupted, stochastic forces create characteristic, observable libration patterns. As a further application, the stochastic migration of small bodies in Saturn’s rings is studied. Analytic predictions of collisional and gravitational interactions of a moonlet with ring particles are compared to realistic three dimensional collisional N-body simulations with up to a million particles. Estimates of both the migration rate and the eccentricity evolution of embedded moonlets are confirmed. The random walk of the moonlet is fast enough to be directly observable by the Cassini spacecraft. Turbulence in the proto-stellar disc also plays an important role during the early phases of the planet formation process. In the core accretion model, small, metre-sized particles are getting concentrated in pressure maxima and will eventually undergo a rapid gravitational collapse to form a gravitationally bound planetesimal. Due to the large separation of scales, this process is very hard to model numerically. A scaled method is presented, that allows for the correct treatment of self-gravity for a marginally collisional system by taking into account the relevant small scale processes. Interestingly, this system is dynamically very similar to Saturn’s rings.

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Becker, John Alex 1964. "Formation and evolution of hypernova progenitors in massive binary systems." Thesis, Massachusetts Institute of Technology, 2004. http://hdl.handle.net/1721.1/28373.

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Thesis (Ph. D.)--Massachusetts Institute of Technology, Dept. of Physics, 2004. Includes bibliographical references (p. 159-170). The massive stellar progenitor of a hypernova explosion and an associated gamma-ray burst must satisfy two primary constraints: (1) the outer layers of the stellar core must possess sufficient angular momentum to form a centrifugally supported torus about the collapsed central object (a Kerr black hole); and, (2) the envelope of the star must not be excessively massive or distended, so that the energetic, ultrarelativistic outflow generated by the central engine in the core of the star does not risk being smothered before it can escape from the star and expand outward to produce a gamma-ray burst. Physical processes which occur during the evolution of an isolated massive star will tend to diminish its initial angular momentum content, rendering it difficult for such a star to become a hypernova progenitor since its core will likely no longer spin rapidly enough to support a torus about its collapsed core. However, a substantial fraction of massive stars are members of binary systems. Tidal locking, mass transfer, or stellar merger in an evolved massive binary system could possibly lead to the transfer of orbital angular momentum to the core of one of the stars (or to the core of a merged star, if a common envelope develops), of sufficient magnitude to produce the core of a successful hypernova progenitor (constraint 1). Further interaction between the stars or their compact remnants could lead to the loss of the hydrogen and possibly helium envelopes of one of the stars (constraint 2). We have developed a new one-dimensional stellar evolution code that includes the effects of rotation on equilibrium stellar structure, and calculates the transport of angular momentum through the stellar interior due to convection, dynamical and secular shear instabilities, and gravity (buoyancy) waves. (cont.) We have used this code to calculate a variety of evolutionary sequences involving the transfer of mass from one component of the binary system to the other. We have also calculated an evolutionary sequence ending in the merger of one component of the system with the core of the other, induced by a prior common-envelope phase. We find that over a wide range of initial binary system parameters, the initially less massive component of the system can accrete a substantial amount of mass and angular momentum from the initially more massive component. The accreted angular momentum is efficiently transported inward from the surface of the accreting star toward its core by a combination of convection and dynamical and secular shear instabilities. If accretion commences while the accretor is still on the main sequence, we find that the inward-progressing wave of angular momentum can penetrate the core of the mass-gaining star, contributing to its store of rotational angular momentum without the need for gravity wave transport of angular momentum across the core- envelope interface. These stars end their evolution (just prior to core carbon ignition) as red supergiants, with cores endowed with sufficient angular momentum to give rise to a hypernova explosion. We also find that a subsequent common-envelope phase with the compact remnant of the primary might result in the ejection of the accretor's red-giant envelope, leaving either a bare helium or carbon-oxygen star. Such a star would be expected to explode in a Type lb or Ic supernova/hypernova. by John Alex Becker. Ph.D.

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17

Brown, David John Alexander. "The effects of tidal interactions on the properties and evolution of hot-Jupiter planetary systems." Thesis, University of St Andrews, 2013. http://hdl.handle.net/10023/4181.

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Thanks to a range of discovery methods that are sensitive to different regions of parameter space, we now know of over 900 planets in over 700 planetary systems. This large population has allowed exoplanetary scientists to move away from a focus on simple discovery, and towards efforts to study the bigger pictures of planetary system formation and evolution. The interactions between planets and their host stars have proven to be varied in both mechanisms and scope. In particular, tidal interactions seem to affect both the physical and dynamical properties of planetary systems, but characterising the broader implications of this has proven challenging. In this thesis I present work that investigates different aspects of tidal interactions, in order to uncover the scope of their influence of planetary system evolution. I compare two different age calculation methods using a large sample of exoplanet and brown dwarf host stars, and find a tendency for stellar model fitting to supply older age estimates than gyrochronology, the evaluation of a star's age through its rotation (Barnes 2007). Investigating possible sources of this discrepancy suggests that angular momentum exchange through the action of tidal forces might be the cause. I then select two systems from my sample, and investigate the effect of tidal interactions on their planetary orbits and stellar spin using a forward integration scheme. By fitting the resulting evolutionary tracks to the observed eccentricity, semi-major axis and stellar rotation rate, and to the stellar age derived from isochronal fitting, I am able to place constraints on tidal dissipation in these systems. I find that the majority of evolutionary histories consistent with my results imply that the stars have been spun up through tidal interactions as the planets spiral towards their Roche limits. I also consider the influence of tidal interactions on the alignment between planetary orbits and stellar spin, presenting new measurements of the projected spin-orbit alignment angle, λ, for six hot Jupiters. I consider my results in the context of the full ensemble of measurements, and find that they support a previously identified trend in alignment angle with tidal timescale, implying that tidal realignment might be responsible for patterns observed in the λ distribution.

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18

Magalhaes, Victor de Souza. "The protosolar nebula heritage : the nitrogen isotopic ratio from interstellar clouds to planetary systems." Thesis, Université Grenoble Alpes (ComUE), 2017. http://www.theses.fr/2017GREAY095/document.

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L'existence de molécules interstellaires soulève une question, ces molécules sont-elles les mêmes molécules que nous voyons dans le système Solaire aujourd'hui ? C'est une question toujours ouverte qui implique des conséquences profondes. Il est possible d’éclaircir cette question en étant capables de retracer l'héritage d'un groupe de molécules chimiquement liées, ce que nous appelons un réservoir. Le meilleur outil pour retracer l'héritage des réservoirs sont les rapports isotopiques. L'élément qui montre les plus grandes variations du rapport isotopique dans le système Solaire est l'azote. Ces variations indiquent que le rapport isotopique de l'azote est sensible aux conditions physiques de la formation des étoiles.L'objectif principal de cette thèse est d'identifier les réservoirs d'azote à différents étapes de la formation des étoiles et des planètes. La première étape de cette entreprise était d'identifier le rapport isotopique de la masse principal d'azote du milieu interstellaire local aujourd'hui.Cela a été déterminé égale à 323 ± 30 à partir du rapport CN/C 15 N mesuré dans le disque protoplanétaire autour de TW Hya. Parallèlement à cela, nous avons également mesuré un rapport HCN/HC 15 N=128 ± 36 dans le disque protoplanétaire autour de MWC 480. Ces rapports isotopiques très distinctes mesurées sur les disques protoplanétaires sont une indication claire de la présence d'au moins deux réservoirs d'azote dans les disques protoplanétaires. La façon dont ces réservoirs se séparent est cependant inconnue. Cela pourrait peut-être se produire en raison de réactions de fractionnement chimique ayant lieu dans les cœurs prestellaires. Nous avions donc comme objectif d'obtenir une mesure précise et directe du rapport isotopique de l'azote des molécules d'HCN dans le cœur prestellaire L1498.Pour obtenir cette mesure, l'obstacle le plus important à surmonter était due aux anomalies hyperfines des molécules d'HCN. Ces anomalies hyperfines sont induites par le chevauchement des composants hyperfins. Ceci sont particulièrement sensibles à la densité de colonne d'HCN, mais aussi au champ de vitesses et aux largeurs de raies. Ainsi les anomalies hyperfines sont un outil de mesure de l'abondance d'HCN permettant aussi de sonder la cinématique des cœurs prestellaires.Pour reproduire avec précision les anomalies hyperfines, et ainsi mesurer des densités de colonne précises d'HCN, nous avions besoin d'explorer un espace de paramètres dégénéré de 15 dimensions. Pour minimiser les dégénérescences nous avons obtenu un profil de densité basé sur des cartes du continuum de L1498. Ceci permettant de réduire à 12 dimensions l'espace des paramètres. L'exploration de cet espace de paramètre a été fait grâce à l'utilisation d'un méthode de minimisation MCMC. Grâce à cette exploration, nous avons obtenu HCN/HC 15 N = 338 ± 28 et HCN/H 13 CN = 45 ± 3. Les incertitudes sur ces valeurs sont limités par les erreurs de calibration et sont dé-terminés de manière non arbitraire par le méthode MCMC. Les implications de ces résultats sont discutées dans le chapitre de conclusion,où nous présentons également quelques perspectives sur l'avenir The existence of interstellar molecules raises the question, are thesemolecules the same molecules we see on the Solar system today? Thisis still an open question with far reaching consequences. Some lightmay be shed on this issue if we are able to trace the heritage of agroup of chemically linked molecules, a so-called reservoir. The besttool to trace the heritage of reservoirs are isotopic ratios. The elementthat shows the largest isotopic ratio variations in the Solar system isnitrogen. For this is an indication that the isotopic ratio of nitrogen issensitive to the physical conditions during star formation.The main objective of this thesis is to identify the reservoirs of ni-trogen at different stages of star and planet formation. The first stepin this endeavour was to identify the isotopic ratio of the bulk of ni-trogen in the local ISM today. This was determined to be 323 ± 30from the CN/C 15 N ratio in the protoplanetary disk around TW Hya.Along with it we also measured the HCN/HC 15 N= 128 ± 36 in theprotoplanetary disk around MWC 480. This very distinct nitrogen iso-topic ratios on protoplanetary disks are a clear indication that thereare at least two reservoirs of nitrogen in protoplanetary disks. Howthese reservoirs get separated is however unknown. This could pos-sibly happen due to chemical fractionation reactions taking place inprestellar cores. We therefore aimed to obtain an accurate direct mea-surement of the nitrogen isotopic ratio of HCN in the prestellar coreL1498.To obtain this measurement the most important hurdle to overcomewere the hyperfine anomalies of HCN. These hyperfine anomaliesarise due to the overlap of hyperfine components. They are especiallysensitive to the column density of HCN, but also to the velocity fieldand line widths. Thus hyperfine anomalies are a tool to measure theabundance of HCN and to probe the kinematics of prestellar cores.To accurately reproduce the hyperfine anomalies, and thus mea-sure accurate column densities for HCN, we needed to explore adegenerate parameter space of 15 dimensions. To minimise the de-generacies we have derived a density profile based on continuummaps of L1498. This reduced the parameter space to 12 dimensions.The exploration of this parameter space was done through the useof a MCMC minimisation method. Through this exploration we ob-tained HCN/HC 15 N = 338 ± 28 and HCN/H 13 CN = 45 ± 3. Theuncertainties on these values are calibration limited and determinednon-arbitrarily by the MCMC method. Implications of these resultsare discussed in the concluding chapter, where we also present somefuture perspectives

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19

Mark, Hannah F. "Seismic and numerical constraints on the formation and evolution of ocean lithosphere." Thesis, Massachusetts Institute of Technology, 2019. https://hdl.handle.net/1721.1/127722.

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Thesis: Ph. D., Joint Program in Oceanography/Applied Ocean Science and Engineering (Massachusetts Institute of Technology, Department of Earth, Atmospheric, and Planetary Sciences; and the Woods Hole Oceanographic Institution), 2019 Cataloged from PDF of thesis. Includes bibliographical references (pages 151-174). This thesis explicates aspects of the basic structure of oceanic lithosphere that are shaped by the processes that form the lithosphere. The strength of lithospheric plates relative to the underlying mantle enables the surface plate motions and plate boundary processes that characterize plate tectonics on Earth. Surprisingly, we have a relatively poor understanding of the physical mechanisms that make the lithosphere strong relative to the asthenosphere, and we lack a reference model for ordinary lithospheric structure that can serve as a baseline for comparing geophysical observations across locations. Chapters 2 and 3 of this thesis investigate the seismic structure of a portion of the Pacific plate where the simple tectonic history of the plate suggests that its structure can be used as a reference model for oceanic lithosphere. We present measurements of shallow azimuthal seismic anisotropy, and of a seismic discontinuity in the upper mantle, that reflect the effects of shear deformation and melting processes involved in the formation of the lithosphere at mid-ocean ridges. Chapter 4 uses numerical models to explore factors controlling fault slip behavior on normal faults that accommodate tectonic extension during plate formation. by Hannah F. Mark. Ph. D. Ph.D. Joint Program in Oceanography/Applied Ocean Science and Engineering (Massachusetts Institute of Technology, Department of Earth, Atmospheric, and Planetary Sciences; and the Woods Hole Oceanographic Institution)

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20

Roberts, Daniel Thomas. "A geomechanical analysis of the formation and evolution of Polygonal Fault Systems." Thesis, Cardiff University, 2014. http://orca.cf.ac.uk/72000/.

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The development of Polygonal Fault Systems (PFS) remains poorly understood despite extensive study for over two decades. These systems of exclusively normal faults are developed over wide areas of many basins worldwide and are believed to influence caprock integrity and hydrocarbon reservoir quality, whilst also potentially presenting shallow drilling hazards. A seemingly obvious conclusion from their layer-bound nature and significant lateral extent is that their origin must be governed by the constitutive behaviour of the host sediments. Establishing specific causative mechanisms has, however, proven difficult. The aim of this research project is to first assess some existing arguments for PFS genesis and this is complimented by a review of modification of structure in soft rocks and discussion of how this facilitates changes in both shear and compaction. The approach in this work is to utilise geomechanical forward modelling to demonstrate how such changes might lead to PFS formation. The concepts of this approach are discussed with focus on the adopted computational framework and selected constitutive model. An argument for polygonal fault genesis is presented that is founded on diagenetically induced shear failure, and the requirements for incorporating this into the constitutive model are described. Recovery of realistic PFS geometries is demonstrated as validation of the geomechanical argument and the competency of the computational approach. Conceptual sensitivity studies at the field scale are undertaken to better understand what processes, reactions and conditions might control fault genesis and propagation. When observed in mapview polygonal faults commonly intersect bedding planes at a wide variety of azimuths which reflects an inferred horizontally isotropic state of stress. Occasionally, this so-called 'planform geometry' is modified by the presence of tectonic faults, slopes or salt structures. Therefore, there is the possibility that polygonal faults may be useful paleostress indicators. This is explored using the characterised materials in simple models featuring anisotropic horizontal stress conditions.

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21

Lyra, Wladimir. "Turbulence-Assisted Planetary Growth : Hydrodynamical Simulations of Accretion Disks and Planet Formation." Doctoral thesis, Uppsala universitet, Institutionen för fysik och astronomi, 2009. http://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-9537.

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The current paradigm in planet formation theory is developed around a hierarquical growth of solid bodies, from interstellar dust grains to rocky planetary cores. A particularly difficult phase in the process is the growth from meter-size boulders to planetary embryos of the size of our Moon or Mars. Objects of this size are expected to drift extremely rapid in a protoplanetary disk, so that they would generally fall into the central star well before larger bodies can form. In this thesis, we used numerical simulations to find a physical mechanism that may retain solids in some parts of protoplanetary disks long enough to allow for the formation of planetary embryos. We found that such accumulation can happen at the borders of so-called dead zones. These dead zones would be regions where the coupling to the ambient magnetic field is weaker and the turbulence is less strong, or maybe even absent in some cases. We show by hydrodynamical simulations that material accumulating between the turbulent active and dead regions would be trapped into vortices to effectively form planetary embryos of Moon to Mars mass. We also show that in disks that already formed a giant planet, solid matter accumulates on the edges of the gap the planet carves, as well as at the stable Lagrangian points. The concentration is strong enough for the solids to clump together and form smaller, rocky planets like Earth. Outside our solar system, some gas giant planets have been detected in the habitable zone of their stars. Their wakes may harbour rocky, Earth-size worlds.

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22

Gaspar, Andras. "Observations and Models of Infrared Debris Disk Signatures and their Evolution." Diss., The University of Arizona, 2011. http://hdl.handle.net/10150/202982.

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In my thesis I investigate the occurrence of mid-infrared excess around stars and their evolution. Since the launch of the first infrared satellite, IRAS, we have known that a large fraction of stars exhibit significant levels of infrared emission above their predicted photospheric level. Resolved optical and infrared images have revealed the majority of these excesses to arise from circumstellar disk structures, made up of distributions of planetesimals, rocks, and dust. These structures are descriptively called debris disks. The first part of my thesis analyzes the Spitzer Space Telescope Observations of δ Velorum. The 24 μm Spitzer images revealed a bow shock structure in front of the star. My analysis showed that this is a result of the star’s high speed interaction with the surrounding interstellar medium. We place this observation and model in context of debris disk detections and the origin of λ Boötis stars. The second part of my thesis summarizes our observational results on the open cluster Praesepe. Using 24 μm data, I investigated the fraction of stars with mid-infrared excess, likely to have debris disks. I also assembled all results from previous debris disk studies and followed the evolution of the fraction of stars with debris disks. The majority of debris disks systems are evolved, few hundred million or a Gyr old. Since the dissipation timescale for the emitting dust particles is less than the age of these systems, they have to be constantly replenished through collisional grinding of the larger bodies. The last two chapters of my thesis is a theoretical analysis of the collisional cascade in debris disks, the process that produces the constant level of dust particles detected. I introduce a numerical model that takes into account all types of destructive collisions in the systems and solves the full scattering equation. I show results of comparisons between my and other published models and extensive verification tests of my model. I also analyze the evolution of the particle size distribution as a function of the variables in my model and show that the model itself is quite robust against most variations.

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23

Wilson, Robert F., Johanna Teske, Steven R. Majewski, et al. "Elemental Abundances of Kepler Objects of Interest in APOGEE. I. Two Distinct Orbital Period Regimes Inferred from Host Star Iron Abundances." IOP PUBLISHING LTD, 2018. http://hdl.handle.net/10150/626528.

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The Apache Point Observatory Galactic Evolution Experiment (APOGEE) has observed similar to 600 transiting exoplanets and exoplanet candidates from Kepler (Kepler Objects of Interest, KOIs), most with >= 18 epochs. The combined multi-epoch spectra are of high signal-to-noise ratio (typically >= 100) and yield precise stellar parameters and chemical abundances. We first confirm the ability of the APOGEE abundance pipeline, ASPCAP, to derive reliable [Fe/H] and effective temperatures for FGK dwarf stars-the primary Kepler host stellar type-by comparing the ASPCAP-derived stellar parameters with those from independent high-resolution spectroscopic characterizations for 221 dwarf stars in the literature. With a sample of 282 close-in (P < 100 days) KOIs observed in the APOGEE KOI goal program, we find a correlation between orbital period and host star [Fe/H] characterized by a critical period, P-crit = 8.3(-4.1)(+0.1) days, below which small exoplanets orbit statistically more metal-enriched host stars. This effect may trace a metallicity dependence of the protoplanetary disk inner radius at the time of planet formation or may be a result of rocky planet ingestion driven by inward planetary migration. We also consider that this may trace a metallicity dependence of the dust sublimation radius, but we find no statistically significant correlation with host T-eff and orbital period to support such a claim.

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Mulders, Gijs D., Ilaria Pascucci, Dániel Apai, Antonio Frasca, and Joanna Molenda-Żakowicz. "A SUPER-SOLAR METALLICITY FOR STARS WITH HOT ROCKY EXOPLANETS." IOP PUBLISHING LTD, 2016. http://hdl.handle.net/10150/622435.

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Host star metallicity provides a measure of the conditions in protoplanetary disks at the time of planet formation. Using a sample of over 20,000 Kepler stars with spectroscopic metallicities from the LAMOST survey, we explore how the exoplanet population depends on host star metallicity as a function of orbital period and planet size. We find that exoplanets with orbital periods less than 10 days are preferentially found around metal-rich stars ([Fe/H] similar or equal to 0.15 +/- 0.05 dex). The occurrence rates of these hot exoplanets increases to similar to 30% for super-solar metallicity stars from similar to 10% for stars with a sub-solar metallicity. Cooler exoplanets, which reside at longer orbital periods and constitute the bulk of the exoplanet population with an occurrence rate of greater than or similar to 90%, have host star metallicities consistent with solar. At short orbital periods, P < 10 days, the difference in host star metallicity is largest for hot rocky planets (< 1.7 R-circle plus), where the metallicity difference is [Fe/H] similar or equal to 0.25 +/- 0.07 dex. The excess of hot rocky planets around metal-rich stars implies they either share a formation mechanism with hot Jupiters, or trace a planet trap at the protoplanetary disk inner edge, which is metallicity dependent. We do not find statistically significant evidence for a previously identified trend that small planets toward the habitable zone are preferentially found around low-metallicity stars. Refuting or confirming this trend requires a larger sample of spectroscopic metallicities.

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25

Horning, Gregory (Gregory William). "Geophysical and geochemical constraints on the evolution of oceanic lithosphere from formation to subduction." Thesis, Massachusetts Institute of Technology, 2017. http://hdl.handle.net/1721.1/108908.

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Thesis: Ph. D., Joint Program in Oceanography/Applied Ocean Science and Engineering (Massachusetts Institute of Technology, Department of Earth, Atmospheric, and Planetary Sciences; and the Woods Hole Oceanographic Institution), 2017. Cataloged from PDF version of thesis. Includes bibliographical references (pages 104-115). This thesis investigates the evolution of the oceanic lithosphere in a broad sense from formation to subduction, in a focused case at the ridge, and in a focused case proximal to subduction. In general, alteration of the oceanic lithosphere begins at the ridge through focused and diffuse hydrothermal flow, continues off axis through low temperature circulation, and may occur approaching subduction zones as bending related faulting provides fluid pathways. In Chapter 2 1 use a dataset of thousands of microearthquakes recorded at the Rainbow massif on the Mid-Atlantic Ridge to characterize the processes which are responsible for the long-term, high-temperature, hydrothermal discharge found hosted in this oceanic core complex. I find that the detachment fault responsible for the uplift of the massif is inactive and that the axial valleys show no evidence for faulting or active magma intrusion. I conclude that the continuous, low-magnitude seismicity located in diffuse pattern in a region with seismic velocities indicating ultramafic host rock suggests that serpentinization may play a role in microearthquake generation but the seismic network was not capable of providing robust focal mechanism solutions to constrain the source characteristics. In Chapter 3 I find that the Juan de Fuca plate, which represents the young/hot end-member of oceanic plates, is lightly hydrated at upper crustal levels except in regions affected by propagator wakes where hydration of lower crust and upper mantle is evident. I conclude that at the subduction zone the plate is nearly dry at upper mantle levels with the majority of water contained in the crust. Finally, in Chapter 4 I examine samples of cretaceous age serpentinite sampled just before subduction at the Puerto Rico Trench. I show that these upper mantle rocks were completely serpentinized under static conditions at the Mid-Atlantic Ridge. Further, they subsequently underwent 100 Ma of seafloor weathering wherein the alteration products of serpentinization themselves continue to be altered. I conclude that complete hydration of the upper mantle is not the end point in the evolution of oceanic lithosphere as it spreads from the axis to subduction. by Gregory Horning. Ph. D.

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26

Pippin, Charles Everett. "Trust and reputation for formation and evolution of multi-robot teams." Diss., Georgia Institute of Technology, 2013. http://hdl.handle.net/1853/50376.

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Agents in most types of societies use information about potential partners to determine whether to form mutually beneficial partnerships. We can say that when this information is used to decide to form a partnership that one agent trusts another, and when agents work together for mutual benefit in a partnership, we refer to this as a form of cooperation. Current multi-robot teams typically have the team's goals either explicitly or implicitly encoded into each robot's utility function and are expected to cooperate and perform as designed. However, there are many situations in which robots may not be interested in full cooperation, or may not be capable of performing as expected. In addition, the control strategy for robots may be fixed with no mechanism for modifying the team structure if teammate performance deteriorates. This dissertation investigates the application of trust to multi-robot teams. This research also addresses the problem of how cooperation can be enabled through the use of incentive mechanisms. We posit a framework wherein robot teams may be formed dynamically, using models of trust. These models are used to improve performance on the team, through evolution of the team dynamics. In this context, robots learn online which of their peers are capable and trustworthy to dynamically adjust their teaming strategy. We apply this framework to multi-robot task allocation and patrolling domains and show that performance is improved when this approach is used on teams that may have poorly performing or untrustworthy members. The contributions of this dissertation include algorithms for applying performance characteristics of individual robots to task allocation, methods for monitoring performance of robot team members, and a framework for modeling trust of robot team members. This work also includes experimental results gathered using simulations and on a team of indoor mobile robots to show that the use of a trust model can improve performance on multi-robot teams in the patrolling task.

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27

RAGUSA, ENRICO. "THE EVOLUTION OF BINARY SYSTEMS IN GASEOUS ENVIRONMENTS." Doctoral thesis, Università degli Studi di Milano, 2018. http://hdl.handle.net/2434/604177.

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Systems where a binary, that is two gravitationally bound objects orbiting their centre of mass, interacts with the surrounding gas or dust are extremely common in the Universe and involve a wide variety of different astrophysical objects (star + star, black hole + black hole, star + planet, or planet + moon). Among them, protoplanetary systems and black hole binaries (BHBs) are currently capturing the attention of the scientific community. Despite their very different nature and EM appearance, both protoplanetary and BHB systems are characterized by the presence of a gaseous accretion disc surrounding the binary. As a consequence, the dynamics of these systems is very similar and can be described in one unique theoretical framework: the disc-satellite interaction theory. This project is meant to deepen our knowledge of the theory of circumbinary discs, approaching it in a multidisciplinary way from both the protoplanetary and the BHBs perspective.

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28

Petit, Antoine. "Architecture et stabilité des systèmes planétaires." Thesis, Paris Sciences et Lettres (ComUE), 2019. http://www.theses.fr/2019PSLEO005.

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L'architecture des systèmes planétaires nous renseigne sur leur formation et de leur histoire. De plus, le grand nombre de découvertes récentes et futures d’exoplanètes permet d’étudier la population de systèmes exoplanétaires. Cependant, l’organisation des systèmes planétaires est fortement affectée par la stabilité dynamique, ce qui rend les études particulièrement difficiles. Étant donné que la dynamique est chaotique, une analyse détaillée entraîne de long temps de calculs. Dans cette thèse, je développe des critères analytiques de stabilité pour la dynamique des planètes. Dans le système séculaire, la conservation du moment cinétique et des demi-grand axes impliquent la conservation du déficit en moment cinétique (AMD). L’AMD est une mesure pondérée des excentricités et des inclinaisons mutuelles d’un système et agit comme une température dynamique. Dans le premier chapitre, nous définissons le concept de d'AMD-stabilité. Le critère d'AMD-stabilité permet de faire la distinction entre les systèmes planétaires a priori stables et les systèmes pour lesquels la stabilité n’est pas garantie et nécessite plus d'études. Je montre que l'AMD-stabilité peut être utilisée pour établir une classification des systèmes multiplanétaires afin de différencier les systèmes stables à long terme et ceux qui sont AMD-instables, nécessitant alors une étude dynamique supplémentaire. Nous classons 131 systèmes multiplanétaires de la base de données exoplanet.eu ayant des éléments orbitaux suffisamment connus. Bien que le critère AMD soit rigoureux, la conservation de l'AMD n’est garantie qu’en l’absence de résonances en moyen mouvement (MMR).Si les îles des MMR se chevauchent, le système devient chaotique et instable.Dans le deuxième chapitre, nous élargissons le critère de stabilité AMD pour prendre en compte le recouvrement de MMR du premier ordre.Je déduis analytiquement un nouveau critère qui unifie ceux précédemment proposés dans la littérature et admet comme cas limite les critères obtenus pour les orbites initialement circulaires et excentriques. Dans le troisième chapitre, j'explique comment la stabilité de Hill peut être comprise via la notion d'AMD. Largement utilisée, la stabilité de Hill est un critère de stabilité topologique pour le système à trois corps.Cependant, la plupart des études utilisent uniquement l'approximation pour des orbites coplanaire et circulaire.Je montre que le critère général de Hill peut être exprimé en fonction des seuls demi-grand axes, des masses et de l'AMD total du système.Le critère proposé n'est développé que dans le rapport de masse des planètes à l'étoile et non dans les éléments orbitaux.Lors de l'étude d'un système AMD-instable, le recours aux simulations numériques est nécessaire. Cependant, les grand temps d'évolution dans la dynamique planétaire rendent nécessaire l'utilisation de méthodes symplectiques. Ces méthodes permettent une intégration très précise et rapide lorsqu'un système est stable. Leur inconvénient est qu'elles sont limités à une intégration à pas de temps fixe, i.e. l'intégrateur peut ne pas résoudre les rencontres proches et devient inexact. Dans le quatrième chapitre, je propose une renormalisation du temps qui permet d’utiliser un intégrateur symplectique d’ordre élevé avec un pas de temps adaptatif aux rencontres proches. L'algorithme est bien adapté aux systèmes de masses de planètes similaires.Dans le dernier chapitre, je revisite le modèle-jouet de formation planétaire de J. Laskar. Tandis que l'AMD est conservé par la dynamique séculaire, il diminue lors des collisions planétaires. Le modèle de Laskar peut être résolu de manière analytique pour obtenir le résultat moyen et les simulations numériques sont très rapides, ce qui permet de créer une grande population de systèmes. Je montre que ce modèle de formation est en bon accord avec les simulations réalistes récentes de formation, dans lesquelles l'architecture finale résulte d'une phase d'impacts géants The architecture of a planetary systems is a signpost of their formation and history.Moreover, the large number of recent and future exoplanets discoveries allows to study the exoplanet system population.Besides, the observations of exoplanet systems has enriched the diversity of planetary system architecture, revealing that the Solar System shape is far from being the norm.However, the organization of planetary systems is heavily affected by dynamical stability, making individual studies particularly challenging.Since planets dynamics are chaotic, a detailed stability analysis study is computationally expensive.In this thesis, I develop analytic stability criteria for planet dynamics.In the secular system, the conservation of the total angular momentum and semi-major axes imply the conservation of the Angular Momentum Deficit (AMD).The AMD is a measure of a system’s eccentricities and mutual inclinations and act as a dynamical temperature of the system.Based on this consideration, we make the simplifying assumption that the dynamics can be replaced by AMD exchanges between the planets.In the first chapter we define the concept of AMD-stability. The AMD-stability criterion allows to discriminate between a priori stable planetary systems and systems for which the stability is not granted and needs further investigations.We show how AMD-stability can be used to establish a classification of the multiplanet systems in order to exhibit theplanetary systems that are long-term stable because they are AMD-stable, and those that are AMD-unstable which then require someadditional dynamical studies to conclude on their stability. We classify 131 multiplanet systems from the exoplanet.eu database with sufficiently well-known orbital elements.While the AMD criterion is rigorous, AMD conservation is only granted in absence of mean-motion resonances (MMR).If the MMR islands overlap, the system experiences chaos leading to instability.In the second chapter, we extend the AMD-stability criterion to take into account the overlap of first-order MMR.I derive analytically a new overlap criterion for first-order MMR.This stability criterion unifies the previous criteria proposed in the literature and admits the criteria obtained for initially circular and eccentric orbits as limit cases.In the third chapter I explain how the Hill stability can be understood in the AMD framework.Widely used, the Hill stability is a topological stability criterion for the three body system.However, most studies only use the coplanar and circular orbit approximation.We show that the general Hill stability criterion can be expressed as a function of only semi-major axes, masses, and total AMD of the system.The proposed criterion is only expanded in the planets-to-star mass ratio and not in the orbital elements.When studying AMD-unstable system, numerical simulations are mandatory.However the long timescales in planet dynamics make necessary the use of symplectic methods.These methods provide very accurate and fast integration when a system is stable.Their downside is that they are limited to fixed time-step integration.For unstable systems, the integrator may fail to resolve a close encounter and become inaccurate.In the fourth chapter, I propose a time renormalization that allow to use high order symplectic integrator with adaptive time-step at close encounter.The algorithm is well-adapted to systems of few similar masses planets.In the final chapter, I revisit the planet formation toy model developed by J. Laskar.While the AMD is conserved in the secular dynamics, it decreases during planets collisions.Laskar's model can be solved analytically for the average outcome and numerical simulations are very quick allowing to build large system population.I show that this formation model is in good agreement with recent realistic planet formation simulations where the final architecture results from a giant impact phase

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29

Bockelée-Morvan, Dominique, J. Crovisier, S. Erard, et al. "Evolution of CO2, CH4, and OCS abundances relative to H2O in the coma of comet 67P around perihelion from Rosetta/VIRTIS-H observations." OXFORD UNIV PRESS, 2016. http://hdl.handle.net/10150/624745.

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Infrared observations of the coma of 67P/Churyumov-Gerasimenko were carried out from 2015 July to September, i.e. around perihelion (2015 August 13), with the high-resolution channel of the Visible and Infrared Thermal Imaging Spectrometer instrument onboard Rosetta. We present the analysis of fluorescence emission lines of H2O, CO2, (CO2)-C-13, OCS, and CH4 detected in limb sounding with the field of view at 2.7-5 km from the comet centre. Measurements are sampling outgassing from the illuminated Southern hemisphere, as revealed by H2O and CO2 raster maps, which show anisotropic distributions, aligned along the projected rotation axis. An abrupt increase of water production is observed 6 d after perihelion. In the meantime, CO2, CH4, and OCS abundances relative to water increased by a factor of 2 to reach mean values of 32, 0.47, and 0.18 per cent, respectively, averaging post-perihelion data. We interpret these changes as resulting from the erosion of volatile-poor surface layers. Sustained dust ablation due to the sublimation of water ice maintained volatile-rich layers near the surface until at least the end of the considered period, as expected for low thermal inertia surface layers. The large abundance measured for CO2 should be representative of the 67P nucleus original composition, and indicates that 67P is a CO2-rich comet. Comparison with abundance ratios measured in the Northern hemisphere shows that seasons play an important role in comet outgassing. The low CO2/H2O values measured above the illuminated Northern hemisphere are not original, but the result of the devolatilization of the uppermost layers.

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30

Zurlo, Alice. "Characterization of exoplanetary systems with the direct imaging technique : towards the first results of SPHERE at the Very Large Telescope." Thesis, Aix-Marseille, 2015. http://www.theses.fr/2015AIXM4721/document.

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Aujourd’hui, plus de 1800 planètes qui orbitent autour d’étoiles en dehors du système solaire ont été découvertes. La plupart des planètes découvertes actuellement a été révélée grâce aux méthodes indirectes. Par contre, avec ce type de techniques, la caractérisation des planètes ne peut pas être complète si on n’utilise pas plusieurs techniques simultanément. Aussi, pour obtenir le spectre de la planète, il doit y avoir un transit et même dans ce cas là,le signal est très faible par rapport au signal de l’étoile. L’observation directe de ces objets, appellée imagerie directe, est maintenant possible grâce à des systèmes très avancés d’optique adaptative installés sur des télescopes de classe 8m. L’imagerie directe permet l’observation des planètes sufisamment lumineuses et éloignées de l’étoile principale en utilisant un masque qui cache la lumière de la dernière. Cette technique est donc efficace en particulier pour des systèmes jeunes et voisins car la luminosité intrinsèque de la planète diminue avec l’âge et la séparation réelle de la planète dépend de la distance du système. Dans le VLT au Paranal (Chili), deux instruments sont dédiés à ce type de recherche : NACO et SPHERE. SPHERE a vu sa première lumière en Mai 2014, et est maintenant prêt à commencer une enquête consacrée à la découverte de planètes autour de systèmes jeunes et voisins, NIRSUR. Cet instrument se compose de trois sous-systèmes : IRDIS, IFS et ZIMPOL In the year of the 20th anniversary of the discovery of the first extrasolar planet we can count more than 1800 companions found with different techniques. The majority of them are indirect methods that infer the presence of an orbiting body by observing the parent star (radial velocity, transits, astrometry). In this work we explore the technique that permits to directly observe planets and retrieve their spectra, under the conditions that they are bright and far enough from their host star. Direct imaging is a new technique became possible thanks to a new generation of extreme adaptive optics instruments mounted on 8m class telescopes. On the Very Large Telescope two instruments dedicated to the research for exoplanets with direct imaging are now operative: NACO and SPHERE. This thesis will describe the development and results of SPHERE from its predecessor NACO to its integration in laboratory and the final on sky results

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31

Allen, Christopher J. T. "Atmospheric mechanisms of central Saharan dust storm formation in boreal summer : observations from the Fennec campaign." Thesis, University of Oxford, 2015. http://ora.ox.ac.uk/objects/uuid:896c26f3-c7a5-4c93-9e53-69b69b28d1cb.

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In boreal summer, satellite measurements show that the central Sahara is the dustiest region of the planet. However, ground-based observations of the central Sahara have been limited to its outer edges, leaving a void in observations approximately 1 million km2 in area. The Fennec Project has been the first campaign to instrument this remote but climatologically important region. This thesis uses these new observations to detect and explain the atmospheric mechanisms that make the central Sahara the summer global dust maximum. Four atmospheric mechanisms are found to cause dust storms in the central Sahara in June 2011 and June 2012. These are cold pool outflows, low-level jets (LLJs), monsoon surges and dry convective plumes. Dust may be emitted locally by these phenomena, or be advected, principally by cold pools. In both field seasons, dust emission by cold pool outflows is the most important dust mechanism, causing roughly half of the total dust loadings at the Fennec supersite of Bordj-Badji Mokhtar (BBM), the closest station to the dust maximum. The second most important mechanism is dust advection by cold pools (roughly 30&percnt; dust at BBM), followed by dust emission by monsoon surges, LLJs and finally dry convective plumes (only 2&percnt; dust at BBM). Although June 2012 was significantly more dusty than June 2011, the relative importance of the different atmospheric dust mechanisms at BBM did not change. At the automatic weather stations (AWSs) across the remote desert, cold pools and LLJs are by far the most frequently detected atmospheric dust mechanisms. LLJs are particularly common in the Atlantic Inflow in western Mauritania and in the north-easterly Harmattan in western Algeria. Cold pools are much more frequent at BBM, the station under the greatest moist monsoon influence, than at the AWSs to the north. Detection of advected dust is a particular difficulty without dedicated dust-detection instrumentation or human observers (e.g. at the AWSs). Detection of dust emission mechanisms can be very successful with only routine ground observations and satellite measurements, but quantifying the associated dust burden without dedicated dust instruments is problematic. The choice of instrumentation for dust measurement is crucial. Because cold pool outflows - the most important dust mechanism - frequently occur at night or under cloud, sun photometers miss about half of cold pool dust. Lidars have the advantage of providing height resolved dust profiles, but they suffer from attenuation in thick dust. The nephelometer proved to be the most reliable dust instrument. Although LLJs occurred on 21/28 mornings at BBM in June 2011, only five of these jets led to dust emission. Calculations of momentum exchanges through the atmospheric column show that momentum mix-down from the jet core is the cause of dust emission on these occasions, but that the LLJ has to be particularly strong (≥ 16 m s-1) to result in dust emission at the surface. Met Office Africa-LAM underestimates monsoon LLJ wind profiles and ERA-Interim reanalysis underestimates both monsoon and Harmattan LLJ wind profiles. At the surface, the Met Office Africa-LAM and GLOBAL models significantly underpredict the frequency of observed wind speeds &gt6 m s-1. This will cause them to significantly underestimate dust emission, as emission is a threshold process proportional to the cube of wind speed. A particularly interesting implication of the research presented here is that the central Sahara is likely much more dusty than previously thought. This is because almost all of the techniques currently used to study dust in the region are systematically biased to result in underestimates of dust burden. Cold pools are the most important dust mechanism but, since they rarely occur during the daytime or in cloud-free conditions they are often missed by sun photometers. Many will be missed by satellites that cannot retrieve below cloud and satellites that pass over the Sahara in daylight hours (e.g. the A-train). A commonly-used satellite dust detection algorithm often misses dust under moist (i.e. cold pool) conditions. Cold pools cannot be simulated by models without explicit convection, which requires very high spatial resolution. Finally, the numerical models assessed here significantly underpredict the frequency of wind speeds over the dust emission threshold. The Sahara is probably much dustier than current estimates suggest.

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32

Mendes, Luana Liberato. "Estabilidade e formação de planetas terrestres em regiões coorbitais /." Guaratinguetá, 2019. http://hdl.handle.net/11449/181758.

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Orientador: Othon Cabo Winter Resumo: Encontrar um planeta como a Terra fora do Sistema Solar parece ser dificil. Quando olhamos para os dados dos quase 4000 exoplanetas descobertos até o momento vemos que nenhum deles é similar à Terra. Uma alternativa para encontrar um outro planeta como a Terra seria olhar para as regiões coorbitais dos exoplanetas gigantes, sendo que sistemas coorbitais podem ser descritos como os sistemas onde dois ou mais corpos compartilham uma mesma órbita média. Nosso objetivo neste trabalho é formar um planeta com a massa da Terra que seja coorbital a um corpo bastante massivo, como um planeta gigante ou uma anã marrom. Para isso nós fizemos várias simulações utilizando o pacote Mercury de integração numérica para o problema de N-corpos. Com os resultados analisamos como a razão de massa do sistema e a separação entre os corpos afetam a região de estabilidade coorbital, e então determinamos seus limites radial e angular. Tendo a região de estabilidade coorbital bem definida para cada um dos sistemas estudados, nós fizemos novas simulações numéricas distribuindo dentro da região de estabilidade coorbital 500 planetesimais que cujas massas somadas totalizam 2 ou 3M⊕. Nossos resultados mostraram que é possível formar planetas terrestres com massas iguais ou maiores que a da Terra nas regiões coorbitais. Esta formação é mais provável para os sistemas cujo corpo secundário possui uma órbita com semi-eixo maior menor que 1ua, sendo que os diferentes valores de razão de massa não afetam o proc... (Resumo completo, clicar acesso eletrônico abaixo) Abstract: Finding an Earth-like planet outside Solar System seems to be a difficult task. When we look at the data from the almost 4000 exoplanets discovered until now we see that none of them is similar to our Earth. An alternative to find other planet like Earth would be to look at the co-orbital regions of the giants exoplanets, being that co-orbital systems can be described as those systems where two or more bodies share the same mean orbit. Our main goal in this work is to form a planet co-orbiting with another massive body, like a giant planet, with the same mass of the Earth. To do that we have performed a series of numerical simulations with the package of computational integrators for the N-body problem called Mercury. With the results we have analyzed how the stable co-orbital region is affected by the system’s mass ratio and by the radial separation between bodies, and then we have determined the radial and angular limits of the stable co-orbital region. Having this region well determined for each one of the studied systems, we have performed new numerical simulations distributing 500 planetesimals within the stable co-orbital region, in which the sum of the planetesimals’s masses are equal to 2 or 3MEarth. Our results have shown that it is possible to form terrestrial planets with masses equals or bigger than the Earth’s inside the stable co-orbital regions. This formation is more likely to happen for the systems in which the secondary body has an orbit with semi-major axis... (Complete abstract click electronic access below) Mestre

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33

Romans, Brian William. "Controls on distribution, timing, and evolution of turbidite systems in tectonically active settings : the cretaceous Tres Pasos Formation, southern Chile, and the Holocene Santa Monica Basin, California /." May be available electronically:, 2008. http://proquest.umi.com/login?COPT=REJTPTU1MTUmSU5UPTAmVkVSPTI=&clientId=12498.

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34

Zurlo, Alice. "Characterization of exoplanetary systems with the direct imaging technique: towards the first results of SPHERE at the Very Large Telescope." Doctoral thesis, Università degli studi di Padova, 2015. http://hdl.handle.net/11577/3424178.

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In the year of the 20th anniversary of the discovery of the first extrasolar planet we can count more than 1800 companions found with different techniques. The majority of them are indirect methods that infer the presence of an orbiting body by observing the parent star (radial velocity, transits, astrometry). In this work we explore the technique that permits to directly observe planets and retrieve their spectra, under the conditions that they are bright and far enough from their host star. Direct imaging is a new technique became possible thanks to a new generation of extreme adaptive optics instruments mounted on 8m class telescopes. On the Very Large Telescope two instruments dedicated to the research for exoplanets with direct imaging are now operative: NACO and SPHERE. This thesis will describe the development and results of SPHERE from its predecessor NACO to its integration in laboratory and the final on sky results. Chapter 1 gives a presentation of the exoplanet research, the formation mechanisms, and the characterization of planet atmospheres. Chapter 2 gives a general frame of the two instruments used for the results presented in this thesis: NACO and SPHERE. In Chapter 3 I describe an example of a false positive in the direct imaging technique, found during the survey NACO-Large Program. This work have been published in Zurlo et al. 2013. In Chapter 4 I present the performance of SPHERE, in particular of the subsystems IRDIS and IFS, deeply tested in the laboratory before the shipping to Paranal. This work has been published in Zurlo et al. 2014. Chapter 5 presents a work done to find special targets for the NIRSUR survey, these object are radial velocity long period planets which are observable with SPHERE. In Chapter 6 I present one of the first on sky result, the observations and analysis of the multi-planetary system HR\,8799. In Chapter 7 I give the conclusions and future prospects. Al giorno d'oggi più di 1800 pianeti sono stati scoperti orbitare attorno a stelle al di fuori del sistema solare. Le tecniche utilizzate per la ricerca di pianeti extrasolari sono molteplici: alcune, dette metodi indiretti, si basano sull'osservazione della perturbazione indotta dal pianeta orbitante sulla stella ospite, mentre altre si basano sull'osservazione diretta del pianeta stesso. La maggior parte dei pianeti scoperti attualmente é stata rivelata grazie ai primi. Specialmente il metodo delle velocità radiali e dei transiti hanno fornito il più alto numero si scoperte. Lo svantaggio di questo tipo di tecniche é che la caratterizzazione del pianeta non può essere completa a meno che non vengano usate simultaneamente più tecniche. Inoltre, per ottenere lo spettro del pianeta, quest'ultimo deve transitare e anche in questo caso il segnale é difficilmente estrapolabile. L'osservazione diretta di questi oggetti, detta “direct imaging”, é oggi possibile grazie ad avanzati sistemi di ottica adattiva installati su telescopi della classe 8m. Il direct imaging permette l'osservazione diretta di pianeti sufficientemente luminosi e distanti dalla stella ospite grazie ad una maschera che oscura la luce di quest'ultima. Questa tecnica quindi é particolarmente efficiente su sistemi giovani e vicini, dato che la luminosità intrinseca del pianeta diminuisce con l'età e che la separazione effettiva del pianeta dipende dalla distanza del sistema stesso. Sul Very Large Telescope a Paranal (Chile) due strumenti sono dedicati a questo tipo di ricerca: NACO e SPHERE. NACO é stato pensato come predecessore e prototipo di SPHERE, ma viene mantenuto grazie alle sue performance ancora competitive ed ad alcune caratteristiche che non sono presenti in SPHERE. SPHERE ha visto la sua prima luce in Maggio 2014 ed é ora pronto per cominciare una survey dedicata alla scoperta di pianeti attorno a sistemi giovani e vicini, NISUR. Questo strumento é composto da tre sottosistemi: IRDIS, IFS e ZIMPOL. IRDIS é una camera infrarossa cui detector é suddiviso in due porzioni uguali per sfruttare l'immagine simultanea del target in due filtri adiacenti. IFS é lo spettrografo di SPHERE, permette di estrarre lo spettro del pianeta con risoluzioni di 30 e 50 a seconda della banda spettrale utilizzata. ZIMPOL é l'unico sottosistema che lavora nel visibile, viene utilizzato per osservare la polarizzazione dei sistemi planetari. In questo lavoro viene presentato lo strumento SPHERE e il suo predecessore NACO, focalizzando sui risultati e sulle performance nella caratterizzazione dei sistemi planetari.

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Cossou, Christophe. "Effet de la structure du disque sur la formation et la migration des planètes." Phd thesis, Université Sciences et Technologies - Bordeaux I, 2013. http://tel.archives-ouvertes.fr/tel-00949904.

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Au delà du système solaire et de ses planètes, nous avons maintenant un catalogue de quasiment 1000 exoplanètes qui illustrent la grande diversité des planètes et des systèmes qu'il est possible de former. Cette diversité est un défi que les modèles de formation planétaire tentent de relever. La migration de type 1 est un des mécanismes pour y parvenir. En fonction des propriétés du disque protoplanétaire, les planètes peuvent s'approcher ou s'éloigner de leur étoile. La grande variété des modèles de disques protoplanétaires permet d'obtenir une grande variété de systèmes planétaires, en accord avec la grande diversité que nous observons déjà pour l'échantillon limité qui nous est accessible. Grâce à des simulations numériques, j'ai pu montrer qu'au sein d'un même disque, il est possible de former des super-Terres ou des noyaux de planètes géantes selon l'histoire de migration d'une population d'embryons.

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Mawet, Dimitri, Élodie Choquet, Olivier Absil, et al. "CHARACTERIZATION OF THE INNER DISK AROUND HD 141569 A FROM KECK/NIRC2 L-BAND VORTEX CORONAGRAPHY." IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/625206.

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HD 141569 A is a pre-main sequence B9.5 Ve star surrounded by a prominent and complex circumstellar disk, likely still in a transition stage from protoplanetary to debris disk phase. Here, we present a new image of the third inner disk component of HD 141569 A made in the L' band (3.8 mu m) during the commissioning of the vector vortex coronagraph that has recently been installed in the near-infrared imager and spectrograph NIRC2 behind the W.M. Keck Observatory Keck II adaptive optics system. We used reference point-spread function subtraction, which reveals the innermost disk component from the inner working distance of similar or equal to 23 au and up to similar or equal to 70 au. The spatial scale of our detection roughly corresponds to the optical and near-infrared scattered light, thermal Q, N, and 8.6 mu m PAH emission reported earlier. We also see an outward progression in dust location from the L' band to the H band (Very Large Telescope/SPHERE image) to the visible (Hubble Space Telescope (HST)/STIS image), which is likely indicative of dust blowout. The warm disk component is nested deep inside the two outer belts imaged by HST-NICMOS in 1999 (at 406 and 245 au, respectively). We fit our new L'-band image and spectral energy distribution of HD 141569 A with the radiative transfer code MCFOST. Our best-fit models favor pure olivine grains and are consistent with the composition of the outer belts. While our image shows a putative very faint point-like clump or source embedded in the inner disk, we did not detect any true companion within the gap between the inner disk and the first outer ring, at a sensitivity of a few Jupiter masses.

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Benbakoura, Mansour. "Evolution des étoiles de faible masse en interaction : observations multi-techniques et modélisation des systèmes multiples." Thesis, Université de Paris (2019-....), 2019. http://www.theses.fr/2019UNIP7027.

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Cette thèse est consacrée à l'étude des étoiles de faible masse ayant dans leur environnement proche d'autres étoiles ou des planètes. Nous nous sommes concentrés sur l'influence des interactions avec ces compagnons sur l'évolution stellaire ainsi que leurs conséquences observables.Dans la première partie, nous présentons le modèle d'évolution des systèmes étoile–planète que nous avons développé au cours de cette thèse, nommé ESPEM (Évolution des Systèmes Planétaires Et Magnétisme). Ce modèle prend en compte de façon ab-initio des effets du vent stellaire magnétisé et de la dissipation de marée sur la rotation stellaire et l'orbite planétaire, simultanément avec l'évolution structurelle de l'étoile. Premièrement, nous l'utilisons pour étudier l'évolution séculaire de la rotation des étoiles hôtes de systèmes planétaires et montrons notamment que cette évolution peut être significativement différente de celle des étoiles isolées. Ensuite, nous examinons les prédictions de ce modèle concernant l'architecture orbitale des systèmes étoile–planète. Nos résultats suggèrent une interprétation aux distributions de périodes orbitales et de de rotation stellaire observées.Dans la deuxième partie, nous montrons en quoi l'observation d'étoiles binaires évoluées permet de tester les théories astrophysiques, notamment l'astérosismologie et l'interaction de marée. Dans un premier temps, nous présentons les résultats d'un programme d'observations que nous avons mené pendant plus de deux ans et qui nous a permis de caractériser 16 systèmes binaires à éclipses. Ensuite, nous comparons ces résultats avec ceux que nous avons obtenus en analysant cet échantillon à l'aide d'outils astérosismiques dans le but de vérifier l'exactitude de ces derniers. Enfin, en élargissant l'échantillon étudié à 30 autres étoiles binaires évoluées, nous testons la théorie de l'évolution de marée. Ceci nous permet à la fois de valider la théorie et de comprendre l'évolution des systèmes observés dans ce travail.Ce travail met en avant deux aspects de la spécificité des systèmes multiples. Premièrement, il montre en quoi l'évolution des étoiles est impactée par la présence d'un compagnon stellaire ou planétaire. Deuxièmement, il met en avant l'intérêt des étoiles binaires pour tester les théories astrophysiques et renforce la compréhension actuelle de l'évolution stellaire This thesis is devoted to the study of low-mass stars having other stars or planets in their immediate environment. We focused on the influence of interactions with these companions on stellar evolution and their observable consequences.In the first part, we present the model of evolution of star–planet systems that we developed during this thesis, called ESPEM (French acronym for Evolution of Planetary Systems and Magnetism). This model incorporates ab-initio prescriptions to quantify the effects of magnetized stellar wind and tidal dissipation on stellar rotation and planetary orbit, simultaneously with the star's structural evolution. First, we use it to study the secular evolution of the rotation of planet-host stars and show that this evolution can be significantly different from that of isolated stars. Next, we examine the predictions of this model regarding the orbital architecture of star–planet systems. Our results suggest an interpretation to the observed distributions of orbital and stellar rotation periods.In the second part of the manuscript, we show how the observation of advanced binary stars allows us to test astrophysical theories, in particular asteroseismology and tidal interaction. First, we present the results of an observation program that we conducted for more than two years and that allowed us to characterize 16 eclipsing binary systems. Then, we compare these results with those obtained by analyzing this sample using asteroseismic tools to verify the accuracy of the latter. Finally, by extending the studied sample to 30 other advanced binary stars including an evolved primary, we test the theory of tidal evolution. This allows us both to validate the theory and to understand the evolution of the systems observed in this work.This work highlights two aspects of the specificity of multiple systems. First, it shows how the evolution of stars is affected by the presence of a stellar or planetary companion. Second, it emphasizes the interest of binary stars in testing astrophysical theories and reinforces the current understanding of stellar evolution

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38

Neves, Vasco. "Étude sur les paramétres stellaires des naines M et leur lien à la formation planétaire." Thesis, Grenoble, 2013. http://www.theses.fr/2013GRENY082/document.

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Au moment d'écrire ma Thèse plus de 900 exoplanètes été annoncées et plus de 2700 planètes détectées par le télescope spatial Kepler sont en attente d'être confirmées. La haute précision des spectres et des courbes de lumière obtenue dans les relevés Doppler et transit, permet l'étude détaillée des paramètres des étoiles hôtes, et ouvre la possibilité d'enquêter sur les corrélations étoile planètes. En outre, la détermination des paramètres stellaires avec précision est un besoin critique pour déterminer les paramètres planétaires, à savoir, la masse, le rayon et la densité.Dans le cas des naines FGK, la détermination des paramètres stellaires est bien établie et peut être utilisée avec confiance pour étudier la relation planète-étoile ainsi que pour obtenir les paramètres planétaires avec une grande precision. Cependant, ce n'est pas le cas pour les naines M, les étoiles les plus communes de la Galaxie. Par rapport à leurs cousines plus chaudes, les naines M sont plus petites, plus froides, et plus faiblement lumineuses, et donc plus difficile à étudier. Le plus grand défi qui concerne les naines M est lié à la présence de milliards de lignes moléculaires qui gomme le continuum et rend l'analyse spectrale classique presque impossible. Trouver des fac ̧ons nouvelles et novatrices pour surmonter cet obstacle et obtenir une mesure des paramètres stellaires est l'objectif principal de cette Thèse .Pour l'atteindre, j'ai concentré mes recherches sur deux approches méthodologiques, photométrique et spectroscopiques. Mon premier travail avait pour objectif d'établir l'étalonnage de métallicité pho- tométrique précis. Par manque de binaires FGK+M avec de bonnes données photométriques je ne pouvais pas atteindre cet objectif. Il m'a cependant était possible, avec les données disponibles, de comparer les étalonnages photométriques déjà établies et légèrement améliorer le meilleur d'entre eux, comme décrit au Chapitre 3.Puis, je me suis concentré sur les approches spectroscopiques pour obtenir des paramètres stel- laires plus précis pour les naines M. À cette fin, j'ai utilisé des spectres HARPS de haute résolution et développé une méthode pour mesurer les lignes spectrales sans tenir compte du continuum . En utilisant cette méthode, je créé un nouvel étalonnage visible avec une précision de 0.08 dex pour [Fe/H] et 80 K pourTeff .Ce travail est détaillé dans le Chapitre 4.Finalement , j'ai également participé à l'amélioration des paramètres de l'étoile GJ3470 et de sa planète, où mon expertise dans les paramètres stellaires de naines M avait un rôle important. Les détails concernant cette enquête sont présentés dans le Chapitre 5 At the time of writing of this Thesis more than 900 planets have been announced and about 2700 planets from the Kepler space telescope are waiting to be confirmed. The very precise spectra and light curves obtained in Doppler and transit surveys, allows the in-depth study of the parameters of the host stars, and opens the possibility to investigate the star-plant correlations. Also, determining the stellar parameters with precision is critical for more precise determinations of the planetary parameters, namely, mass, radius, and density.In the case of the FGK dwarfs, the determination of stellar parameters is well established and can be used with confidence to study the star-planet relation as well as to obtain precise planetary parameters. However, this is not the case for M dwarfs, the most common stars in the Galaxy. Compared to their hotter cousins, M dwarfs are smaller, colder, and fainter, and therefore harder to study. The biggest challenge regarding M dwarfs is related to the presence of billions of molecular lines that depress the continuum making a classical spectral analysis almost impossible. Finding new and innovative ways to overcome this obstacle in order to obtain precise stellar parameters is the goal of this Thesis.To achieve this goal I focused my research into two main avenues: photometric and spectroscopic methods. My initial work had the objective of establishing a precise photometric metallicity calibration, but I could not reach this goal, as I did not have enough FGK+M binaries with good photometric data. However, it was possible, with the available data, to compare the already established photometric calibrations and slightly improve the best one, as described in Chapter 3.Then, I focused on spectroscopic approaches with the aim of obtaining precise M dwarf parame- ters. To this end I used HARPS high-resolution spectra and developed a method to measure the spectral lines disregarding the continuum completely. Using this method I established a new visible calibration with a precision of 0.08 dex for [Fe/H] and 80 K for Te f f . This work is detailed in Chapter 4.Finally, I also participated in the refinement of the parameters of the star GJ3470 and its planet, where my expertise in stellar parameters of M dwarfs had an important role. The details regarding this investigation are shown in Chapter 5 No momento em que escrevo esta Tese, o número de planetas anunciados já ultrapassou os 900 e os cerca de 2700 candidatos detectados pelo telescópio espacial Kepler esperam por confirmação. Os espectros e as curvas de luz obtidos nos programas de procura de planetas permitem, também, o estudo em profundidade dos parâmetros das estrelas com planetas e abrem a possibilidade de investigar a relação estrela-planeta. Neste contexto, a determinação com precisão dos parâmetros estelares é crítica na determinação precisa dos parâmetros planetários, nomeadamente, a massa, o raio e a densidade.No caso das anãs FGK, os métodos de determinação dos parâmetros estelares estão bem estabelecidos e podem ser usados com confiança no estudo da relação estrela-planeta, assim como na obtenção de parâmetros planetários precisos. No entanto, não é esse o caso para as anãs M, as estrelas mais comuns da nossa Galáxia. Ao contrário das suas primas, as estrelas M são mais pequenas, frias e ténues e, assim sendo, mais difíceis de estudar. O grande entrave no estudo das estrelas M está relacionado com a presença de biliões de linhas moleculares que deprimem o contínuo espectral, fazendo com que uma análise espectral clássica se torne quase impossível. A procura de métodos inovadores que possibilitem ultrapassar este obstáculo, tendo em vista a obtenção de parâmetros precisos, é o objectivo desta Tese.Tendo em conta esse objetivo, foquei os meus esforços em duas linhas principais de pesquisa, baseadas em métodos fotométricos e métodos espectroscópicos. O meu trabalho inicial tinha como objetivo o estabelecimento de uma calibração fotométrica para a metalicidade, mas não me foi possível atingir esse objetivo, pois não tinha sistemas binários FGK+M suficientes com bons dados fotométricos. No entanto, foi possível, com os dados disponíveis, comparar as calibrações fotométricas existentes e refinar ligeiramente a melhor delas, como descrito no Capítulo 3.Após este trabalho passei a concentrar-me em técnicas espectroscópicas de obtenção de parâmetros estelares em estrelas M. Tendo em mente esse objetivo, usei espectros HARPS de alta resolução para desenvolver um novo método de medição de linhas espectrais independente do contínuo espectral. Seguidamente, usei este método no desenvolvimento de uma nova calibração de metalicidade e temperatura efectiva em estrelas M na região do visível, através da qual consegui atingir uma precisão de 0.08 dex para a [Fe/H] e de 80 K para a temperatura. Este trabalho está descrito no Capítulo 4.Ao mesmo tempo colaborei na determinação com precisão dos parâmetros da estrela GJ3470 e do seu planeta, onde a minha proficiência na determinação de parâmetros estelares em anãs M teve um papel importante. Os detalhes relacionados com este trabalho de investigação estão descritos no Capítulo 5

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39

Lebreton, Jérémy. "Observations et modélisation des systèmes planétaires autour des étoiles proches." Phd thesis, Université de Grenoble, 2013. http://tel.archives-ouvertes.fr/tel-00952803.

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Les disques de débris orbitant dans l'environnement des étoiles proches constituent un indicateur très important des propriétés des systèmes planétaires extra-solaires. Depuis l'espace et au sol, les moyens observationnels actuels permettent de déterminer dans divers domaines de longueurs d'ondes les propriétés spatiales de ces disques et celles des grains de poussières circumstellaires. Cette thèse aborde le sujet de la modélisation des disques de débris, à partir de données fournies par de multiples instruments, en premier lieu les télescopes spatiaux Hubble et Herschel, et les interféromètres infrarouges du VLTI, CHARA, et KIN. Mes premiers projets ont pris place dans le cadre de deux programmes-clés de l'Observatoire Spatial Herschel dédiés à l'étude des disques circumstellaires autour des étoiles proches. Au sein du projet GASPS, j'ai obtenu des observations spectro-photométriques de HD 181327, une jeune étoile (12+8-4 millions d'années, Ma) de type solaire entourée d'un anneau de débris massif de 90 unités astronomique (UA) de rayon vu aussi en lumière diffusée par le télescope spatial Hubble. La bonne détermination de la géométrie de l'anneau permet de se concentrer sur la modélisation de la distribution spectrale d'énergie, afin de mieux caractériser les propriétés des poussières. J'ai utilisé le code de transfert radiatif GRaTer et démontré que le système héberge une population de planétésimaux glacés, qui pourrait représenter une source d'eau et de volatils susceptible d'être libérée sur des planètes telluriques encore en formation. Je discute quelques résultats additionnels obtenus avec Herschel à propos de disques de débris jeunes, notamment HD 32297, et d'analogues faibles de la Ceinture de Kuiper. Les disques exo-zodiacaux (exozodis), analogues du nuage Zodiacal du Système Solaire, représentent une contrepartie chaude (ou tiède) aux disques de débris, résidant proche de la zone habitable (moins de quelques unités astronomiques) et encore mal connue. Ils sont révélés par leur émission proche et moyen infrarouge et peuvent être étudiés avec la précision et la résolution requises grace à l'interférométrie optique. Dans le cas de l'étoile Beta Pictoris (12+8-4 Ma), dont le disque est vu par la tranche, une fraction significative du disque externe diffuse de la lumière vers le champ de vue des interféromètres ; une composante interne chaude doit tout de même être invoquée pour justifier de l'excès mesuré dans l'infrarouge proche. En m'appuyant sur l'exemple de l'étoile Véga (440±40 Ma), je présente la méthodologie employée et démontre que les exozodis chauds se caractérisent par une abondance de poussières sub-microniques, près de la distance de sublimation de l'étoile. D'un point de vue théorique, le mécanisme de production de ces petits grains non-liés est encore incompris. J'aborde plus en détails le cas du disque exozodiacal à deux composantes (chaude et tiède) de Fomalhaut (440±40 Ma). Je développe une nouvelle méthode de calcul des distances de sublimation et recense les processus variés qui peuvent affecter un grain de poussière afin de fournir un cadre pour l'interprétation : l'exozodi chaud à ~0.1 - 0.2 UA serait la signature indirecte d'une ceinture d'astéroïdes située à 2 UA à l'activité dynamique particulièrement intense. Finalement, je dresse un bilan des propriétés des disques de débris et de ce qu'ils peuvent nous apprendre quand on les compare au Système Solaire, et propose de futures directions de recherche pour explorer davantage les systèmes planétaires et leur dynamique.

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40

Ortiz, Mauricio, Sabine Reffert, Trifon Trifonov, et al. "Precise radial velocities of giant stars." EDP SCIENCES S A, 2016. http://hdl.handle.net/10150/622444.

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Context. For over 12 yr, we have carried out a precise radial velocity (RV) survey of a sample of 373 G- and K-giant stars using the Hamilton Echelle Spectrograph at the Lick Observatory. There are, among others, a number of multiple planetary systems in our sample as well as several planetary candidates in stellar binaries. Aims. We aim at detecting and characterizing substellar and stellar companions to the giant star HD 59686 A (HR 2877, HIP 36616). Methods. We obtained high-precision RV measurements of the star HD 59686 A. By fitting a Keplerian model to the periodic changes in the RVs, we can assess the nature of companions in the system. To distinguish between RV variations that are due to non-radial pulsation or stellar spots, we used infrared RVs taken with the CRIRES spectrograph at the Very Large Telescope. Additionally, to characterize the system in more detail, we obtained high-resolution images with LMIRCam at the Large Binocular Telescope. Results. We report the probable discovery of a giant planet with a mass of m(p) sin i = 6.92(-0.24)(+0.18) M-Jup orbiting at a(p) = 1.0860(-0.0007)(+0.0006) aufrom the giant star HD 59686 A. In addition to the planetary signal, we discovered an eccentric (e(B) = 0.729(-0.003)(+0.004)) binary companionwith a mass of m(B) sin i = 0.5296(-0.0008)(+0.0011) M-circle dot orbiting at a close separation from the giant primary with a semi-major axis of a(B) = 13.56(-0.14)(+0.18) au. Conclusions. The existence of the planet HD 59686 Ab in a tight eccentric binary system severely challenges standard giant planet formation theories and requires substantial improvements to such theories in tight binaries. Otherwise, alternative planet formation scenarios such as second-generation planets or dynamical interactions in an early phase of the system's lifetime need to be seriously considered to better understand the origin of this enigmatic planet.

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41

Kollmeier, Juna Ariele. "The intergalactic medium absorption, emission, disruption /." Columbus, Ohio : Ohio State University, 2006. http://rave.ohiolink.edu/etdc/view?acc%5Fnum=osu1153856075.

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42

Laporte, Nicolas. "Recherche et étude des premières galaxies." Phd thesis, Université Paul Sabatier - Toulouse III, 2012. http://tel.archives-ouvertes.fr/tel-00781144.

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L'évolution des galaxies est relativement bien contrainte jusqu'au premier milliard d'années de l'Univers. Au delà de cette limite et compte-tenu du faible nombre de sources confirmées à z>6.0, il est difficile de déterminer le rôle joué par les premières galaxies à cette époque. L'objectif de ce travail de thèse était de déterminer l'évolution de la fonction de luminosité des galaxies au cours du premier milliard d'années en se basant sur un échantillon représentatif d'objets à grand redshift (z>4.5) suffisamment brillant pour être observé par les spectrographes actuels. Dans ce but, nous avons réalisé une sélection photométrique ciblée de galaxies à cassure de Lyman dans deux champs de vue : un premier autour de l'amas de galaxies d'Abell 2667 et un second dans un très grand champ vide (le relevé WUDS). L'étude des données prises autour d'Abell 2667 a montré un taux de contamination d'environ 80% de notre échantillon d'objets à z≈8. Nous avons mis en évidence l'existence d'une population atypique de galaxies fortement rougies par la poussière à z≈2, et qui ne peuvent être écartées des échantillons qu'en ajoutant des contraintes dans l'IR lointain. Les observations spectroscopiques ont permis d'identifier un nouveau type de contaminant à bas redshift combinant deux populations stellaires d'âges très différents, et demandant une profondeur photométrique extrême afin de les exclure des échantillons actuels. A partir des échantillons dégagés nous avons pu apporter des contraintes fortes et indépendantes sur la partie brillante de la fonction de luminosité, et ainsi en déduire de façon homogène son évolution au cours du premier milliard d'années de l'Univers.

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43

Garcia, Thomas. "Déterminants évolutionnistes de la socialité : le rôle de la formation de groupe." Phd thesis, Université Pierre et Marie Curie - Paris VI, 2013. http://tel.archives-ouvertes.fr/tel-01018209.

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Les interactions collectives, quoique récurrentes chez les microbes, sont paradoxales du point de vue de la sélection naturelle : les traits individuels qui les sous-tendent sont coûteux, donc sujets à l'exploitation de " tricheurs ". Parmi les modèles théoriques, la plupart privilégient des formalismes statiques et idéalisés, et négligent les processus physiques de formation de groupes. Dans une 1ère partie, je décris un cadre formel général pour modéliser les dynamiques évolutives d'un trait social qui augmente la propension à interagir et la cohésion des groupes. Je prouve que la meilleure agrégation des sociaux (attachement différentiel) leur suffit à s'assortir sans besoin de capacités de reconnaissance mutuelle, allégeant l'hypothèse d'attachement préférentiel fréquemment invoquée dans la littérature en l'absence de sélection de parentèle. Dans une 2nde partie, j'étaye cette preuve de principe en spécifiant un modèle computationnel d'agrégation où les individus exercent les uns sur les autres des forces d'interaction d'intensité dépendant de leur type. Je montre que l'émergence et le maintien de la socialité sont compatibles avec de tels processus de formation de groupes, en détaillant à quelles conditions sur les paramètres écologiques et microscopiques. Ce travail constitue une suggestion de scénario mécaniste pour l'évolution de la socialité au sein de groupes de taille arbitraire, ne requérant ni capacités cognitives pour les individus ni apparentement génétique. Il se veut éclairant sur les déterminants évolutionnistes de la structure sociale d'organismes tels que les dictyostélides et les myxobactéries, ainsi que sur les origines possibles de la multicellularité.

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44

Saker, Leila Yamila. "Material circunestelar en estrellas de tipo enanas blancas." Doctoral thesis, 2020. http://hdl.handle.net/11086/23533.

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Tesis (Doctor en Astronomía)--Universidad Nacional de Córdoba, Facultad de Matemática, Astronomía, Física y Computación, 2020. Se han descubierto discos de gas en un grupo de enanas blancas con discos de polvo, a través de la detección en sus espectros de lineas de emisión inusuales del triplete de Ca II en 8600 Å. En este contexto, se han obtenido espectros ópticos GMOS/GEMINI para 13 enanas blancas con excesos IR, seleccionados de nuestra muestra de 29 estrellas con discos “debris”, con el objetivo de encontrar la contraparte gaseosa a los discos de polvo. Se presenta además un estudio comparativo de las principales propiedades físicas y de parámetros relacionados al disco de polvo de las enanas blancas con y sin discos de gas detectados. Adicionalmente, se aplicó la técnica de “Eclipse Timing Variation” en una muestra de 8 sistemas binarios eclipsantes formados por enana blanca+estrella de secuencia principal con el objetivo de detectar planetas circumbinarios. Para ello, se obtuvieron observaciones propias con los telescopios argentinos localizados en la Estación Astrofísica de Bosque Alegre y el telescopio Jorge Sahade en el Complejo Astronómico El Leoncito. Las curvas de luz obtenidas, fueron complementadas con las disponibles en las bases de datos del “Catalina Sky Survey” y Kepler+K2. Los tiempos de mínimo fueron obtenidos con el código Wilson & Devinney. Gas disks have been discovered in a group of white dwarfs with dust disks, through the detection in their spectra of unusual emission lines of the triplet of Ca II at 8600 Å. In this context, GMOS/GEMINI optical spectra have been obtained for 13 white dwarfs with IR excesses, selected from our sample of 29 stars with debris disks, with the aim to find the gaseous counterpart to the dusty disks. We also present a comparative study of the main physical properties and parameters related to the dusty disk of white dwarfs with and without gas disks detected. Additionally, the Eclipse Timing Variation technique was applied in a sample of 8 eclipsing binary systems formed by white dwarf + main sequence star, with the aim to detect circumbinary planets. For this, own observations were obtained with the Argentine telescopes located in the Estación Astrofísica de Bosque Alegre and the Jorge Sahade telescope in the Complejo Astronómico El Leoncito. The light curves obtained were complemented with those available in the databases "Catalina Sky Survey" and Kepler+K2. Minimum times were obtained with the Wilson & Devinney code. Fil: Saker, Leila Yamila. Universidad Nacional de Córdoba. Facultad de Matemática, Astronomía, Física y Computación; Argentina.

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45

Brugamyer, Erik John. "Silicon and oxygen abundances in planet-host stars." Thesis, 2010. http://hdl.handle.net/2152/ETD-UT-2010-12-2303.

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The positive correlation between planet detection rate and host star iron abundance lends strong support to the core accretion theory of planet formation. However, iron is not the most significant mass contributor to the cores of giant planets. Since giant planet cores grow from silicate grains with icy mantles, the likelihood of gas giant formation should depend heavily on the oxygen and silicon abundance of the planet formation environment. Here we compare the silicon and oxygen abundances of a set of 60 planet hosts and a control sample of 60 metal-rich stars without giant planets. We find a 99% probability that planet detection rate depends on the silicon abundance of the host star, over and above the observed planet-metallicity correlation. Due to our large error bars on oxygen abundances, we do not yet observe any correlation between oxygen abundance and planet detection rate. We predict that a correlation between planet occurrence and oxygen abundance should emerge when we can measure [O/Fe] at 0.05 dex precision. Since up to 20% of the carbon in the universe may be in refractory grains, we also predict that planet detection rate should correlate positively with host star carbon abundance for any population of planets formed by core accretion. text

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46

SHERIDAN, EMILY. "Dynamical Evolution and Growth of Protoplanets Embedded in a Turbulent Gas Disk." Thesis, 2009. http://hdl.handle.net/1974/5163.

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Simulations were performed to determine the effect of turbulence on protoplanets as they accrete inside of a planetary gas disk at the stage of planet formation that involves interactions between relatively large, similar sized bodies. The effect of turbulence was implemented into an existing N-Body code using a parameterization of magnetohydrodynamic (MHD) turbulence performed by Laughlin et. al. (2004). The investigation focussed on the effect of turbulent perturbations on planetary dynamics and accretion at various locations in the disk, particularly at large semimajor axis. At these distances, protoplanet collisions are generally less frequent due to the large induced eccentricities from close encounters and due to the trapping of protoplanets in mutual resonances. It is, however, essential that large protoplanets develop at these distances since some must eventually grow large enough to accrete the massive gas envelopes indicative of the giant planets. The interaction between a protoplanet and the surrounding gas disk creates a torque imbalance acting on the protoplanet, which is generally believed to result in the rapid inward spiraling of the protoplanet. In order to create a fixed region in the disk within which protoplanets may interact without migrating into the central star, two scenarios were considered that would inhibit the inward migration of the protoplanets. The first scenario involved a gas disk that had been truncated at the inner edge, referred to as a planet trap, and the second involved the existence of a stationary giant planet within a gap in the disk, referred to as a planet barrier. Each scenario was tested using different density profiles of the gas disk, different numbers and masses of initial protoplanets, various rates of gas disk decay and also four different levels of turbulence intensities. The results demonstrated that the addition of turbulence to the gas disk promotes planet mixing and results in an increased number of collisions between planets, even at large heliocentric distances. A turbulent disk has the tendency to create a final system where the planets are, on average, larger than those produced in a non-turbulent disk. Thesis (Master, Physics, Engineering Physics and Astronomy) -- Queen's University, 2009-09-17 14:41:52.607

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47

Mudryk, Lawrence Russell. "Planetary system evolution: Planet-disk interactions and planet ejection from binary systems." 2007. http://link.library.utoronto.ca/eir/EIRdetail.cfm?Resources__ID=742500&T=F.

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48

Carelli, Fabio. "Molecular anions in circumstellar envelopes, interstellar clouds and planetary atmospheres: quantum dynamics of formation and evolution." Doctoral thesis, 2011. http://hdl.handle.net/11573/918878.

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Nowadays, it is a well known fact that most of the matter in our Solar System, in our Galaxy and, probably, within the whole Universe, exists in the form of ionized particles. For decades astronomers and astrophysicists believed that only positively charged ions were worthy of relevance in drawing the networks for possible chemical reactions in the interstellar medium, as well as in modeling the physical conditions in most of astrophysical environments. Thus, negative ions (and especially molecular negative ions) received minor attention until their possible existence was observationally confirmed (discovery of the first interstellar anion, C6H-), about thirty years after the first physically reasonable proposal on their actual detection was theoretically surmised by E.Herbst (1981). From a purely theoretical point of view, negatively charged ions play a peculiar role as they can be formed in large quantities in the gas phase by attachment of low (1.5 eV < E < 10 eV) and very low-energy (E < 1.5 eV) free electrons, while sometimes such a formation process can occur even close to zero eV. In an astrophysical context, roughly speaking, their role should be then found in their involvement in the charge balance as well as in the chemical evolution of the considered environment: depending on their amount and on the global gas density, in fact, the possible evolutive scenario could be susceptible of marked variations on the estimated time needed for reaching the steady state, their presence having thus also important repercussions on the final chemical composition of a given environment. In contrast, the formation of positive ions requires an energy amount equal to or greater than the first ionization potential of the neutral molecular species considered, i.e. an energy around 8-10 eV for most of organic molecules, a value which is considerably high for several astronomical contexts, like cold dense interstellar molecular clouds and, with less importance, within diffuse molecular gaseous regions. Low-energy electrons, usually considered in the 0-10 eV range, can be very reactive in the sense that they are effectively captured by many molecules, which can then undergo either rapid stabilization toward the undissociated species or fast unimolecular decomposition toward specific fragments, where, in the latter case, the extra electron initially captured by the neutral molecular target, can in turn remain stuck to one of the fragments as well as be re-emitted again in the surroundings with a different (usually lower) kinetic energy. Consequently, it can play a role in heating the gaseous medium at a molecular level. Furthermore, low-energy electrons can also be ’simply’ deflected and then causing vibro-rotational excitation of the target molecules, therefore, playing once more a role in the heating processes at a molecular level. On a much larger scale, they could even produce conductivity inhomogeneity, which in turn disturbs the radiowave propagation in such a medium, like on the edge or on the tail of an interstellar shock, or in principle also moving across a dense cloud: from this point of view, electrons can be also seen as an important and versatile source for ’decoupling’, at least in the low frequency range, the energy transfer from the interstellar radiative field to molecules and nanoparticles. Hence, in a qualitative sense, all of these nanoscopic mechanisms could play a crucial role in understanding more deeply the local interactions within different ’phases’ of the ISM, ranging from the cold dense molecular gas up to the diffuse molecular component. In fact, if we look at the stars, with high energy thermonuclear burning reactions in their interiors, as the primary sources of almost all the energy that is released in the seemingly empty interstellar space, then we can look at the free electrons as a flexible ’means’ which, in competition with photons, is able to participate into the complex processes responsible for the coupling between the ionized, the dust and the neutral components of the ISM. Generally speaking, the main reasons that originally motivated us to undertake the present work, were at least two. First of all, we intended to demonstrate the importance of resonances in forming molecular anions in different astrophysical environments. Secondly, we were attracted by the possibility of investigating with a reliable and suitably approximate approach, the occurrence of radiationless paths like intramolecular vibrational redistributions (IVRs) to account for the dissipation of the extra energy initially carried by the impinging electron. The former aim, which is of course a common feature to each of the molecules investigated here, can be easily justified on the basis of the most important attempts recently dedicated to the understanding of anion formation processes in several astrophysical environments, where indeed only s-wave electron attachment processes were expressly considered. In the framework of the electron-molecule collisions, once the physical conditions like the mean free electron density and the mean kinetic electron temperature are defined according to the specific astronomical context under investigation, taking in consideration only s-wave electron attachment processes to account for the formation of molecular anions provides, in fact, a reliable but narrow point of view. In a qualitative sense, resonant electron attachment can be viewed as the doorway for the ensuing possible formation of the stable molecular anion, provided that the neutral molecule has a positive electron affinity. It therefore follows that the resonant contributions associated to partial waves referred to non-spherical angular momentum states, can account for the formation of molecular anions also for non-vanishing collision energies which can be still relevant in the given environment. In this framework, once one has determined which are the astrophysically relevant resonances for a given molecule, it becomes of interest to also investigate which is the possible evolution of those resonant species: the radiative stabilization for the extra energy content that characterizes the resonant species, in fact, is usually a slow process, that can even exceeds the resonance’s lifetime, so that in such a case the autodetachment becomes strongly competitive. On the other hand, the radiationless IVR constitutes in general another reliable evolutive path that, conversely to the spontaneous emission of a 'high-energy' photon, can efficiently lead to the stabilization of the metastable anion; at the same time, according to the non-ergodic vibrational redistribution, which for a pletora of molecules is an actual possibility, such a process can also account for specific fragmentation channels, as will be shown in details in the last chapter, where all the findings shall be analised and discussed. The present PhD thesis is focusing on electron-molecule interactions with astrophysically relevant molecules, and therefore represents a theoretical/computational work which deals with an area placed at the boundary between (molecular) astrophysics, quantum collision thery, and of course theoretical chemistry. The three molecular species that will be computationally investigated for their behaviour under low-energy electron collisions are the ortho-benzyne (o-C6H4), the coronene (C24H12), and the carbon nitride (NC2N), respectively. Due to their sizes, their peculiar structures, their chemical reactivity and their physical and chemical properties as well as according to astronomical observations, when available, the above three molecules provide representative examples for different astrophysical contexts. However, each of them is linked to a specific astrophysical aspect that currently constitutes an intriguing scientific challenge, hence the present study.

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49

Kratter, Kaitlin Michelle. "Accretion Disks and the Formation of Stellar Systems." Thesis, 2010. http://hdl.handle.net/1807/26283.

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In this thesis, we examine the role of accretion disks in the formation of stellar systems, focusing on young massive disks which regulate the flow of material from the parent molecular core down to the star. We study the evolution of disks with high infall rates that develop strong gravitational instabilities. We begin in chapter 1 with a review of the observations and theory which underpin models for the earliest phases of star formation and provide a brief review of basic accretion disk physics, and the numerical methods which we employ. In chapter 2 we outline the current models of binary and multiple star formation, and review their successes and shortcomings from a theoretical and observational perspective. In chapter 3 we begin with a relatively simple analytic model for disks around young, very massive stars, showing that instability in these disks may be responsible for the higher multiplicity fraction of massive stars, and perhaps the upper mass to which they grow. We extend these models in chapter 4 to explore the properties of disks and the formation of binary companions across a broad range of stellar masses. In particular, we model the role of global and local mechanisms for angular momentum transport in regulating the relative masses of disks and stars. We follow the evolution of these disks throughout the main accretion phase of the system, and predict the trajectory of disks through parameter space. We follow up on the predictions made in our analytic models with a series of high resolution, global numerical experiments in chapter 5. Here we propose and test a new parameterization for describing rapidly accreting, gravitationally unstable disks. We find that disk properties and system multiplicity can be mapped out well in this parameter space. Finally, in chapter 6, we address whether our studies of unstable disks are relevant to recently detected massive planets on wide orbits around their central stars.

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50

"The Diversity of Chemical Composition and the Effects on Stellar Evolution and Planetary Habitability." Doctoral diss., 2017. http://hdl.handle.net/2286/R.I.45482.

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abstract: I present a catalog of 1,794 stellar evolution models for solar-type and low-mass stars, which is intended to help characterize real host-stars of interest during the ongoing search for potentially habitable exoplanets. The main grid is composed of 904 tracks, for 0.5-1.2 M_sol at scaled metallicity values of 0.1-1.5 Z_sol and specific elemental abundance ratio values of 0.44-2.28 O/Fe_sol, 0.58-1.72 C/Fe_sol, 0.54-1.84 Mg/Fe_sol, and 0.5-2.0 Ne/Fe_sol. The catalog includes a small grid of late stage evolutionary tracks (25 models), as well as a grid of M-dwarf stars for 0.1-0.45 M_sol (856 models). The time-dependent habitable zone evolution is calculated for each track, and is strongly dependent on stellar mass, effective temperature, and luminosity parameterizations. I have also developed a subroutine for the stellar evolution code TYCHO that implements a minimalist coupled model for estimating changes in the stellar X-ray luminosity, mass loss, rotational velocity, and magnetic activity over time; to test the utility of the updated code, I created a small grid (9 models) for solar-mass stars, with variations in rotational velocity and scaled metallicity. Including this kind of information in the catalog will ultimately allow for a more robust consideration of the long-term conditions that orbiting planets may experience. In order to gauge the true habitability potential of a given planetary system, it is extremely important to characterize the host-star's mass, specific chemical composition, and thus the timescale over which the star will evolve. It is also necessary to assess the likelihood that a planet found in the "instantaneous" habitable zone has actually had sufficient time to become "detectably" habitable. This catalog provides accurate stellar evolution predictions for a large collection of theoretical host-stars; the models are of particular utility in that they represent the real variation in stellar parameters that have been observed in nearby stars. Dissertation/Thesis Doctoral Dissertation Astrophysics 2017

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Дисертації з теми "Formation and evolution of planetary systems"

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