Bibliografie tematiche / Formation and evolution of planetary systems

Letteratura scientifica selezionata sul tema "Formation and evolution of planetary systems"

Autore: Grafiati

Pubblicato: 8 giugno 2024

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Articoli di riviste sul tema "Formation and evolution of planetary systems":

Burke, Bernard F. "Planetary systems: Formation, evolution, and detection - introduction". Astrophysics and Space Science 212, n. 1-2 (febbraio 1994): xi—xii. http://dx.doi.org/10.1007/bf00984502.

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Horedt, G. P. "The Formation and evolution of planetary systems". Physics of the Earth and Planetary Interiors 67, n. 3-4 (luglio 1991): 392–94. http://dx.doi.org/10.1016/0031-9201(91)90035-g.

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Owen, Tobias. "The formation and evolution of planetary systems". Icarus 91, n. 2 (giugno 1991): 334–35. http://dx.doi.org/10.1016/0019-1035(91)90029-s.

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Lipschutz, Michael E. "The formation and evolution of planetary systems". Geochimica et Cosmochimica Acta 54, n. 4 (aprile 1990): 1196. http://dx.doi.org/10.1016/0016-7037(90)90455-t.

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Kley, Wilhelm. "Formation and Orbital Evolution of Planets". Proceedings of the International Astronomical Union 7, S282 (luglio 2011): 429–36. http://dx.doi.org/10.1017/s1743921311027980.

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AbstractThe formation of planetary systems is a natural byproduct of the star formation process. Planets can form inside the protoplanetary disk by two alternative processes. Either through a sequence of sticking collisions, the so-called sequential accretion scenario, or via gravitational instability from an over-dense clump inside the protoplanetary disk. The first process is believed to have occurred in the solar system. The most important steps in this process will be outlined. The observed orbital properties of exoplanetary systems are distinctly different from our own Solar System. In particular, their small distance from the star, their high eccentricity and large mass point to the existence of a phase with strong mutual excitations. These are believed to be a result of early evolution of planets due to planet-disk interaction. The importance of this process in shaping the dynamical structure of planetary systems will be presented.

Veras, Dimitri. "Post-main-sequence planetary system evolution". Royal Society Open Science 3, n. 2 (febbraio 2016): 150571. http://dx.doi.org/10.1098/rsos.150571.

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The fates of planetary systems provide unassailable insights into their formation and represent rich cross-disciplinary dynamical laboratories. Mounting observations of post-main-sequence planetary systems necessitate a complementary level of theoretical scrutiny. Here, I review the diverse dynamical processes which affect planets, asteroids, comets and pebbles as their parent stars evolve into giant branch, white dwarf and neutron stars. This reference provides a foundation for the interpretation and modelling of currently known systems and upcoming discoveries.

Lin, D. N. C. "Planetary Formation in Protostellar Disks". International Astronomical Union Colloquium 163 (1997): 321–30. http://dx.doi.org/10.1017/s0252921100042792.

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AbstractRecent discoveries of planets around other stars suggest that planets are ubiquitous and their dynamical properties are diverse. We reviewed the formation mechanism for protoplanets and the post-formation planet-disk tidal interaction which may have led the short-period planets to their present configuration. We suggest that these planets may be the survivors of a populations of similar planets which have plunged into and contaminated the stellar convection zone. In the context of the solar system, the mass of the giant planets and the present distribution of the minor planets may be used to infer the structure and evolution for the primordial solar nebula. The large eccentricity of 70 Vir and HD 114762 may be due to cohesive collisions in planetary systems which become unstable during their long term orbital evolution.

Marzari, Francesco, e Philippe Thebault. "Planets in Binaries: Formation and Dynamical Evolution". Galaxies 7, n. 4 (16 ottobre 2019): 84. http://dx.doi.org/10.3390/galaxies7040084.

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Binary systems are very common among field stars, yet the vast majority of known exoplanets have been detected around single stars. While this relatively small number of planets in binaries is probably partly due to strong observational biases, there is, however, statistical evidence that planets are indeed less frequent in binaries with separations smaller than 100 au, strongly suggesting that the presence of a close-in companion star has an adverse effect on planet formation. It is indeed possible for the gravitational pull of the second star to affect all the different stages of planet formation, from proto-planetary disk formation to dust accumulation into planetesimals, to the accretion of these planetesimals into large planetary embryos and, eventually, the final growth of these embryos into planets. For the crucial planetesimal-accretion phase, the complex coupling between dynamical perturbations from the binary and friction due to gas in the proto-planetary disk suggests that planetesimal accretion might be hampered due to increased, accretion-hostile impact velocities. Likewise, the interplay between the binary’s secular perturbations and mean motion resonances lead to unstable regions, where not only planet formation is inhibited, but where a massive body would be ejected from the system on a hyperbolic orbit. The amplitude of these two main effects is different for S- and P-type planets, so that a comparison between the two populations might outline the influence of the companion star on the planet formation process. Unfortunately, at present the two populations (circumstellar or circumbinary) are not known equally well and different biases and uncertainties prevent a quantitative comparison. We also highlight the long-term dynamical evolution of both S and P-type systems and focus on how these different evolutions influence the final architecture of planetary systems in binaries.

Kawai, Toshio. "Pattern Formation by Inelastic Collisions, Especially in Planetary Systems". International Journal of Modern Physics B 12, n. 03 (30 gennaio 1998): 309–60. http://dx.doi.org/10.1142/s0217979298000247.

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The Titius–Bode law governs the planet distribution in our Solar system. In this paper a possible explanation is proposed based on inelastic collision effects among planetessimals during the evolution of the Solar system. The main purpose of this paper is, however, to introduce a strategy to study phenomena driven by rare but drastic events such as colllisions in the planetary problem. Many complex systems evolve through rare but violent events, so that an efficient strategy to simulate such systems is desirable. An event-driven strategy is proposed in this article, and is used to produce many runs of 108 year evolution history of planetary systems. I have found that the Titius–Bode law holds approximately, if the gravitational effect (scattering) and the collisions are taken into account. The result illustrates the importance of inelastic collisions, which are often neglected in the standard classical mechanics courses. Therefore, for completeness, other simpler particle systems under the effect of inelastc collisions, such as one-dimensional systems, are also included.

Salnikova, T. V., S. Ya Stepanov e E. I. Kugushev. "Possible models of the planetary systems formations". International Journal of Modern Physics A 35, n. 02n03 (30 gennaio 2020): 2040061. http://dx.doi.org/10.1142/s0217751x20400618.

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We discuss extended model of planetary system formation. Gravitational collapse of protoplanets leads to the formation of planets and their satellite systems. We consider the hypothesis of a two-stage mechanism of formation of satellite system. Small satellites are formed from the remnants of a collapsing protoplanetary cloud, and large satellites are formed by capturing other relatively small protoplanets. In this paper we study the process of formation of the initial gas-dust cloud, whose evolution leads to the formation of a protoplanetary, and then a planetary system. The justification of the extended model is carried out by numerical simulation. Stable for some time configurations are obtained as a result of interaction of the oncoming mass flows: the spatial collisionless matter takes a lens-like shape, and the planar dissipative system tends to form two gravitating rotating bodies, like the binary stars.

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Tesi sul tema "Formation and evolution of planetary systems":

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

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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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.

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.

Meng, Huan Y. A., George H. Rieke, Kate Y. L. Su e 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.

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.

Ngo, Henry, Heather A. Knutson, Sasha Hinkley, Marta Bryan, Justin R. Crepp, Konstantin Batygin, Ian Crossfield 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.

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

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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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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Più fonti

Libri sul tema "Formation and evolution of planetary systems":

Burke, Bernard F., Jürgen H. Rahe e Elizabeth E. Roettger, a cura di. Planetary Systems: Formation, Evolution, and Detection. Dordrecht: Springer Netherlands, 1994. http://dx.doi.org/10.1007/978-94-011-1154-6.

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Formation and Evolution of Planetary Systems Meeting (1988 Baltimore, Md.). The formation and evolution of planetary systems: Proceedings of the Formation and Evolution of Planetary Systems Meeting, Baltimore, 1988, May 9-11. Cambridge: Cambridge University Press, 1989.

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N, Kylafis, e Lada Charles J, a cura di. The Origin of stars and planetary systems. Boston, Mass: Kluwer Academic, 1999.

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J, Lada Charles, Kylafis N e NATO Advanced Study Institute on the Physics of Star Formation and Early Stellar Evolution (2nd : 1998 : Crete, Greece), a cura di. The origin of stars and planetary systems. Dordrecht: Kluwer Academic Publishers, 1999.

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United States. National Aeronautics and Space Administration., a cura di. Formation of the giant planets by concurrent accretion of solids and gas: Final technical report : grant number: NAG2-984. [Washington, DC: National Aeronautics and Space Administration, 1997.

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1928-, Burke Bernard F., Rahe Jürgen H. Rahe e Roettger Elizabeth E, a cura di. Planetary systems: Formation, evolution, and detection : proceedings of the first international conference, held in Pasadena, California on December 8-10, 1992. Dordrecht: Kluwer Academic, 1994.

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Packevich, Alla. Architecture of Evolution. ru: INFRA-M Academic Publishing LLC., 2021. http://dx.doi.org/10.12737/1079356.

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Abstract (sommario):

The monograph, on the one hand, examines the period of development of the descending cycle of evolution and the associated progressive changes that show the irreversibility of the processes of formation of the planetary system. The end of one cycle and the beginning of another leads to the transformation of the system of life and the expansion of consciousness at a new energy level. On the other hand, the questions of potential opportunities for the development of the ascending phase of evolution, which goes both along the path of complexity of the organization and along the path of diversity, are considered. In the ascending evolutionary stream, what has been differentiated into the corresponding levels in the descending cycle is brought together and thus prepared to enter into new, more perfect forms of unity. It is shown that the development of humanity along its entire path depends on the interaction of energies of various forms and potentials. Understanding the relationships between different types of energy and their use provides insight into many important issues in the evolution of society. The material introduces the modern features of the existence of the male and female sexes from the energy point of view. The idea of a way out of the current conflict situation that has arisen between the sexes at the present stage of evolution is proposed. It will be useful for those interested in the problems of scientific knowledge, architects, philosophers,historians, physicists and methodologists of science, students and students of secondary schools.

Symposium, International Astronomical Union. The astrophysics of planetary systems: Formation, structure, and dynamical evolution : proceedings of the 276th Symposium of the International Astronomical Union, held in Torino, Italy, October 10-15, 2010. Cambridge, U.K: Cambridge University Press, 2011.

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Symposium, International Astronomical Union. Planetary systems in the universe: Observation, formation and evolution : proceedings of the 202nd Symposium of the International Astronomical Union held at University of Manchester, Manchester, United Kingdom, August 7-10, 2000. [San Francisco, Calif.]: Published on behalf of the IAU by Astronomical Society of the Pacific, 2004.

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Dvorak, R., e J. Henrard, a cura di. Long Term Evolution of Planetary Systems. Dordrecht: Springer Netherlands, 1988. http://dx.doi.org/10.1007/978-94-009-2285-3.

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Capitoli di libri sul tema "Formation and evolution of planetary systems":

Bonsor, Amy, e Siyi Xu. "White Dwarf Planetary Systems: Insights Regarding the Fate of Planetary Systems". In Formation, Evolution, and Dynamics of Young Solar Systems, 229–52. Cham: Springer International Publishing, 2017. http://dx.doi.org/10.1007/978-3-319-60609-5_8.

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Safronov, V. S., e E. L. Ruskol. "Formation and Evolution of Planets". In Planetary Systems: Formation, Evolution, and Detection, 13–22. Dordrecht: Springer Netherlands, 1994. http://dx.doi.org/10.1007/978-94-011-1154-6_2.

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Fierro, J. "Interaction of Planetary Nebulae with Prenebulae Debris". In Planetary Systems: Formation, Evolution, and Detection, 61–65. Dordrecht: Springer Netherlands, 1994. http://dx.doi.org/10.1007/978-94-011-1154-6_8.

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Cruikshank, D. P., M. W. Werner e D. E. Backman. "SIRTF: Capabilities for the Study of Planetary Systems". In Planetary Systems: Formation, Evolution, and Detection, 407–15. Dordrecht: Springer Netherlands, 1994. http://dx.doi.org/10.1007/978-94-011-1154-6_42.

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Donn, Bertram, e J. Mark Duva. "Formation and Properties of Fluffy Planetesimals". In Planetary Systems: Formation, Evolution, and Detection, 43–47. Dordrecht: Springer Netherlands, 1994. http://dx.doi.org/10.1007/978-94-011-1154-6_5.

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Wetherill, George W. "Possible Consequences of Absence of “Jupiters“ in Planetary Systems". In Planetary Systems: Formation, Evolution, and Detection, 23–32. Dordrecht: Springer Netherlands, 1994. http://dx.doi.org/10.1007/978-94-011-1154-6_3.

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Sargent, A. I., e S. V. W. Beckwith. "The Detection and Study of Pre-Planetary Disks". In Planetary Systems: Formation, Evolution, and Detection, 181–89. Dordrecht: Springer Netherlands, 1994. http://dx.doi.org/10.1007/978-94-011-1154-6_20.

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Owen, T. "The Search for Other Planets: Clues from the Solar System". In Planetary Systems: Formation, Evolution, and Detection, 1–11. Dordrecht: Springer Netherlands, 1994. http://dx.doi.org/10.1007/978-94-011-1154-6_1.

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Peale, S. J. "On the Detection of Mutual Perturbations as Proof of Planets Around PSR1257+12". In Planetary Systems: Formation, Evolution, and Detection, 77–89. Dordrecht: Springer Netherlands, 1994. http://dx.doi.org/10.1007/978-94-011-1154-6_10.

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Phillips, J. A., e S. E. Thorsett. "Planets Around Pulsars: A Review". In Planetary Systems: Formation, Evolution, and Detection, 91–106. Dordrecht: Springer Netherlands, 1994. http://dx.doi.org/10.1007/978-94-011-1154-6_11.

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Atti di convegni sul tema "Formation and evolution of planetary systems":

Grady, C. A., Michael E. Van Steenberg, George Sonneborn, H. Warren Moos e William P. Blair. "Planetary System Formation and Evolution: The FUSE Legacy and Future FUV Potential". In FUTURE DIRECTIONS IN ULTRAVIOLET SPECTROSCOPY: A Conference Inspired by the Accomplishments of the Far Ultraviolet Spectroscopic Explorer Mission. AIP, 2009. http://dx.doi.org/10.1063/1.3154058.

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Marov, M. Ya, e I. I. Shevchenko. "Planets — a modern view". In ASTRONOMY AT THE EPOCH OF MULTIMESSENGER STUDIES. Proceedings of the VAK-2021 conference, Aug 23–28, 2021. Crossref, 2022. http://dx.doi.org/10.51194/vak2021.2022.1.1.005.

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Abstract (sommario):

The modern view of planets goes far beyond the usual concept of the planets as bodies of the Solar system. The discovery ofexoplanets has immeasurably expanded the understanding of the architecture and properties of planetary systems. Majoradvances have been made in the study of the planets and minor bodies of the Solar system. However, no answers havebeen received to fundamental questions about the causes of various paths of evolution and formation of planetary naturalcomplexes. To give answers to these questions, research on exoplanets is called upon, of which more than 5000 have beendiscovered to date. Exoplanet studies provide an approach to solving the key problems of stellar-planetary cosmogony —the genesis and evolution of planets as byproduct of star formation. The most urgent problems concern the formation ofplanetary systems around stars of various spectral classes; the nature of hot Jupiters; the reasons for the predominanceof super-Earths and sub-Neptunes, which are absent in the Solar system; stability of planetary systems of binary stars,including circumbinary systems. Of particular interest are terrestrial planets with orbits in zones of “potential habitability”,studies of which open a new page in astrobiology.

Otsuka, M., H. Izumiura, A. Tajitsu, S. Hyung, Takuma Suda, Takaya Nozawa, Akira Ohnishi et al. "The Origin and Evolution of the Extremely Metal-Poor Halo Planetary Nebulae". In ORIGIN OF MATTER AND EVOLUTION OF GALAXIES: The 10th International Symposium on Origin of Matter and Evolution of Galaxies: From the Dawn of Universe to the Formation of Solar System. AIP, 2008. http://dx.doi.org/10.1063/1.2943614.

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Abdulmyanov, T. "Comparison of the dynamics of Jupiter’s coorbital asteroids and the dynamics of bodies in debris disks". In ASTRONOMY AT THE EPOCH OF MULTIMESSENGER STUDIES. Proceedings of the VAK-2021 conference, Aug 23–28, 2021. Crossref, 2022. http://dx.doi.org/10.51194/vak2021.2022.1.1.018.

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Abstract (sommario):

The mechanisms of fragmentation of the equatorial dust disk around young stars and the formation of planetary systemsare considered. Using the model of librational motions of co-orbital asteroids of Jupiter, a model of viscous motion of gas,dust particles and small bodies in dust disks is constructed. The dynamic viscosity is obtained from the Navier-Stokesequation for three cases of characteristic ﬂow orbits.It is shown that the librational orbits of Trojans at the early stages ofthe evolution of planetary systems could be transit orbits for dust particles during the formation of celestial bodies of smalland large sizes and masses.

Athanassoula, E. "Formation and Dynamical Evolution of Galaxies and of their Components". In PLANETARY NEBULAE AS ASTRONOMICAL TOOLS: International Conference on Planetary Nebulae as Astronomical Tools. AIP, 2005. http://dx.doi.org/10.1063/1.2146306.

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Chiappini, Cristina. "Low and Intermediate Mass Stars as Tools to Understand Stellar Evolution and the Formation of the Milky Way". In PLANETARY NEBULAE AS ASTRONOMICAL TOOLS: International Conference on Planetary Nebulae as Astronomical Tools. AIP, 2005. http://dx.doi.org/10.1063/1.2146288.

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Savage, Paul, e Frédéric Moynier. "Planetary formation and evolution through the lens of zinc and copper isotopes". In Goldschmidt2023. France: European Association of Geochemistry, 2023. http://dx.doi.org/10.7185/gold2023.20371.

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Rein, Hanno, John C. B. Papaloizou, Tomonori Usuda, Motohide Tamura e Miki Ishii. "Formation of Multi-planetary Systems in Turbulent Disks". In EXOPLANETS AND DISKS: THEIR FORMATION AND DIVERSITY: Proceedings of the International Conference. AIP, 2009. http://dx.doi.org/10.1063/1.3215915.

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Bonsor, Amy, e Mark C. Wyatt. "Post-Main Sequence Evolution of Debris Discs". In PLANETARY SYSTEMS BEYOND THE MAIN SEQUENCE: Proceedings of the International Conference. AIP, 2011. http://dx.doi.org/10.1063/1.3556183.

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