Relevant bibliographies by topics / Stellar astronomy and planetary systems

Academic literature on the topic 'Stellar astronomy and planetary systems'

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Published: 10 December 2022
Last updated: 28 January 2023

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Journal articles on the topic "Stellar astronomy and planetary systems"

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Kouwenhoven, M. B. N., Francesco Flammini Dotti, Qi Shu, Xiuming Xu, Kai Wu, Xiaoying Pang, and Wei Hao. "Planetary systems in dense stellar environments." Journal of Physics: Conference Series 1523 (April 2020): 012011. http://dx.doi.org/10.1088/1742-6596/1523/1/012011.

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Terzian, Yervant. "Distances of Planetary Nebulae." Symposium - International Astronomical Union 155 (1993): 109–21. http://dx.doi.org/10.1017/s0074180900170287.

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One of the most fundamental physical parameter in astronomy is the distance to the objects we detect in the universe. For many classes of astronomical objects, accurate and proven methods have been developed to determine their distances. Such classes of objects include stars within ∼100 pc from the sun, binary stellar systems, variable stars, stellar clusters, main sequence stars, and other galaxies. It has been, however, more difficult to develop satisfactory methods to determine accurate distances to the more than 1000 planetary nebulae that have been discovered in our galaxy.
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Fukushima, Toshio, Jan Vondrák, Nicole Capitaine, George A. Krasinsky, Andrea Milani, Imants Platais, Veronique Dehant, and Demetrios N. Matsakis. "DIVISION I: FUNDAMENTAL ASTRONOMY." Proceedings of the International Astronomical Union 3, T26B (December 2007): 71–73. http://dx.doi.org/10.1017/s1743921308023673.

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Division I provides a focus for astronomers studying a wide range of problems related to fundamental physical phenomena such as time, the inertial reference frame, positions and proper motions of celestial objects, and precise dynamical computation of the motions of bodies in stellar or planetary systems in the Universe.
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Vondrák, Jan, Dennis D. McCarthy, Toshio Fukushima, Aleksander Brzezinski, Joseph A. Burns, Pascale Defraigne, Dafydd Wyn Evans, et al. "DIVISION I: FUNDAMENTAL ASTRONOMY." Proceedings of the International Astronomical Union 4, T27A (December 2008): 1–4. http://dx.doi.org/10.1017/s1743921308025222.

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Division I provides a focus for astronomers studying a wide range of problems related to fundamental physical phenomena such as time, the inertial reference frame, positions and proper motions of celestial objects and precise dynamical computation of the motions of bodies in stellar or planetary systems in the Universe.
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Milani, Andrea, Joseph A. Burns, J. Hadjidemetriou, Z. Knežević, C. Beaugé, B. Erdi, T. Fukushima, et al. "COMMISSION 7: Celestial Mechanics and Dynamical Astronomy." Proceedings of the International Astronomical Union 1, T26A (December 2005): 7–16. http://dx.doi.org/10.1017/s1743921306004297.

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The orbital fits of multi-planetary systems from radial velocity data has proved to be a complex task. In some cases, different orbital solutions provide similarly good fits, especially when two planets are near mean-motion resonances. Ferraz-Melloet al(2005) and Goździewskiet al(2005) showed that the published best fits of systemsHD82932andHD160691are dynamically unstable, and re-determined their orbital parameters with Monte Carlo and genetic algorithms. In both cases dynamically stable orbits were found with RMS similar to the published orbits. It was also shown that uncertainties in the stellar mass Ferraz Melloet al(2005) and the stellar jitter Gozdziewskiet al(2005) can significantly affect the orbital determination. Ford (2005) used a Markov chain Monte Carlo technique to quantify the orbit uncertainties. For some planetary systems he found a strong correlation between the orbital elements and/or significant non-Gaussian error distribution in the parameter space. As a consequence, the actual uncertainties in the orbital fits can be much larger (or smaller) than those published.
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Mal’nev, A. G., V. V. Orlov, and A. V. Petrova. "The dynamical evolution of stellar-planetary systems." Astronomy Reports 50, no. 5 (May 2006): 405–10. http://dx.doi.org/10.1134/s106377290605009x.

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Niedzielski, Andrzej, Grzegorz Nowak, and Paweł Zieliński. "The PSU/TCfA search for planets around evolved stars. Stellar parameters and activity indicators of targets." Proceedings of the International Astronomical Union 3, S249 (October 2007): 49–52. http://dx.doi.org/10.1017/s1743921308016359.

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AbstractThe main objective of the Penn State/Toruń Centre for Astronomy search for planets around evolved stars is the detection of planetary systems around massive, evolved stars. We are also interested in the evolution of these systems on stellar evolution timescales. In this paper we present our approach to determine the basic physical parameters of our targets GK-giants. We also discuss the stellar activity indicators used in our survey: line bisector and curvature, and Hα variability.
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Le Bars, M., L. Lacaze, S. Le Dizès, P. Le Gal, and M. Rieutord. "Tidal instability in stellar and planetary binary systems." Physics of the Earth and Planetary Interiors 178, no. 1-2 (January 2010): 48–55. http://dx.doi.org/10.1016/j.pepi.2009.07.005.

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Adibekyan, V., N. C. Santos, O. D. S. Demangeon, J. P. Faria, S. C. C. Barros, M. Oshagh, P. Figueira, et al. "Stellar clustering and orbital architecture of planetary systems." Astronomy & Astrophysics 649 (May 2021): A111. http://dx.doi.org/10.1051/0004-6361/202040201.

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Context. Revealing the mechanisms shaping the architecture of planetary systems is crucial for our understanding of their formation and evolution. In this context, it has been recently proposed that stellar clustering might be the key in shaping the orbital architecture of exoplanets. Aims. The main goal of this work is to explore the factors that shape the orbits of planets. Methods. We performed different statistical tests to compare the properties of planets and their host stars associated with different stellar environments. Results. We used a homogeneous sample of relatively young FGK dwarf stars with radial velocity detected planets and tested the hypothesis that their association to phase space (position-velocity) over-densities (“cluster” stars) and under-densities (“field” stars) impacts the orbital periods of planets. When controlling for the host star properties on a sample of 52 planets orbiting around cluster stars and 15 planets orbiting around field stars, we found no significant difference in the period distribution of planets orbiting these two populations of stars. By considering an extended sample of 73 planets orbiting around cluster stars and 25 planets orbiting field stars, a significant difference in the planetary period distributions emerged. However, the hosts associated with stellar under-densities appeared to be significantly older than their cluster counterparts. This does not allow us to conclude as to whether the planetary architecture is related to age, environment, or both. We further studied a sample of planets orbiting cluster stars to study the mechanism responsible for the shaping of orbits of planets in similar environments. We could not identify a parameter that can unambiguously be responsible for the orbital architecture of massive planets, perhaps, indicating the complexity of the issue. Conclusions. An increased number of planets in clusters and in over-density environments will help to build large and unbiased samples which will then allow to better understand the dominant processes shaping the orbits of planets.
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Flammini Dotti, Francesco, M. B. N. Kouwenhoven, Maxwell Xu Cai, and Rainer Spurzem. "Planetary systems in a star cluster I: the Solar system scenario." Monthly Notices of the Royal Astronomical Society 489, no. 2 (August 23, 2019): 2280–97. http://dx.doi.org/10.1093/mnras/stz2346.

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ABSTRACTYoung stars are mostly found in dense stellar environments, and even our own Solar system may have formed in a star cluster. Here, we numerically explore the evolution of planetary systems similar to our own Solar system in star clusters. We investigate the evolution of planetary systems in star clusters. Most stellar encounters are tidal, hyperbolic, and adiabatic. A small fraction of the planetary systems escape from the star cluster within 50 Myr; those with low escape speeds often remain intact during and after the escape process. While most planetary systems inside the star cluster remain intact, a subset is strongly perturbed during the first 50 Myr. Over the course of time, $0.3\!-\!5.3{{\ \rm per\ cent}}$ of the planets escape, sometimes up to tens of millions of years after a stellar encounter occurred. Survival rates are highest for Jupiter, while Uranus and Neptune have the highest escape rates. Unless directly affected by a stellar encounter itself, Jupiter frequently serves as a barrier that protects the terrestrial planets from perturbations in the outer planetary system. In low-density environments, Jupiter provides protection from perturbations in the outer planetary system, while in high-density environments, direct perturbations of Jupiter by neighbouring stars is disruptive to habitable-zone planets. The diversity amongst planetary systems that is present in the star clusters at 50 Myr, and amongst the escaping planetary systems, is high, which contributes to explaining the high diversity of observed exoplanet systems in star clusters and in the Galactic field.
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Dissertations / Theses on the topic "Stellar astronomy and planetary systems"

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Soto, Vásquez Maritza Gabriela. "Detection and characterization of single and double stellar/planetary systems." Tesis, Universidad de Chile, 2018. http://repositorio.uchile.cl/handle/2250/159571.

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Doctora en Ciencias, Mención Astronomía
El crecimiento exponencial del número de exoplanetas descubiertos en los últimos años ha derivado en un mayor entendimiento de los planetas en la galaxia, de los cuales la Tierra es miembro; pero aún nos queda un gran camino por delante. El propósito de esta tesis es descubrir y confirmar nuevos planetas orbitando estrellas enanas y gigantes, además de desarrollar técnicas para extraer la mayor cantidad de información posible de las estrellas, permitiendo así una mayor compresión de los sistemas planetarios en estudio. Primero, analizamos datos crudos tomados con FEROS de las estrellas HD 11977, HD 47536, HD 110014, y HD122430, todas con al menos un planeta descubierto. Confirmamos la existencia de los planetas orbitando a HD 11977, HD 47536 y HD 110012, pero con parámetros orbitales distintos a los publicados. Además, no encontramos evidencia que respaldara la existencia del segundo planeta orbitando a HD 47536, ni que hubiese planetas alrededor de HD 122430 y HD 70573. Finalmente, reportamos el descubrimiento de un segundo planeta orbitanto a HD 110014, con una masa mínima de 3.1 \mjup y periodo orbital de 130 días. Luego, usando datos fotométricos de la campaña 11 y 12 de la misión K2, junto con mediciones de velocidad radial tomados con los espectrógrafos HARPS, FEROS, y Coralie, reportamos el descubrimiento de dos planetas Jupiter calientes orbitando a dos estrellas enanas. Encontramos que K2-237 b y K2-238 b tienen masas de $1.36^{+0.10}_{-0.10}$ y $0.86^{+0.13}_{-0.12}$ \mjup, radio de $1.63^{+0.07}_{-0.08}$ y $1.30^{+0.15}_{-0.14}$ \rjup, y orbitan a sus estrellas con órbitas de 1.28 y 3.2 días, respectivamente. El gran tamaño de K2-237 b nos lleva a concluir que corresponde a un Jupiter caliente altamente inflado, mientras que el radio de K2-238 b es consistente con modelos teóricos. K2-237 b representa un excelente laboratorio para estudios de atmósferas planetarias. Finalmente, desarrollamos una herramiento que permite el cálculo automático de parámetros estelares para grandes cantidades de estrellas, usando espectros echelle de alta resolución. SPECIES mide anchos equivalentes para un gran número de líneas de fierro y los usa para resolver la ecuación de transferencia radiativa asumiento equilibrio termodinámico local para obtener los párametros atmosféricos. Estos valores son usados para obtener la abundancia de 11 elementos químicos en las atmósferas estelares. La velocidad de rotación y de macroturbulencia son obtenidos usando fórmulas calibradas a la temperatura estelar, y perfiles de línea sintéticos que igualen a los perfiles medidos para cinco líneas de absorción. SPECIES obtiene la masa, radio y edad interpolando en isocronas MIST, usando el método Bayesiano. Luego de una serie de pruebas encontramos que los parámetros que obtiene SPECIES son congruentes con los de la literatura. También derivamos relaciones analíticas que describen las correlaciones entre los parámetros, e implementamos nuevos métodos para trabajar con estas correlaciones en la obtención de las incertezas asociadas a cada medición.
Este trabajo ha sido parcialmente financiado por CONICYT-PCHA/Doctorado Nacional/2014-21141037
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Burke, Christopher J. "Survey for transiting extrasolar planets in stellar systems stellar and planetary content of the Open Cluster NGC 1245 /." Columbus, Ohio : Ohio State University, 2005. http://rave.ohiolink.edu/etdc/view?acc%5Fnum=osu1132168623.

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Schröter, Sebastian [Verfasser], and Jürgen H. M. M. [Akademischer Betreuer] Schmitt. "Analysis of Stellar Activity and Orbital Dynamics in Extrasolar Planetary Systems / Sebastian Schröter. Betreuer: Jürgen H. M. M. Schmitt." Hamburg : Staats- und Universitätsbibliothek Hamburg, 2012. http://d-nb.info/1024355306/34.

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Bruno, Giovanni. "Characterization of transiting exoplanets : analyzing the impact of the host star on the planet parameters." Thesis, Aix-Marseille, 2015. http://www.theses.fr/2015AIXM4746/document.

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Dans le cadre de ma thèse, j’ai analysé les spectres de neuf étoiles Kepler obtenus avec les relevés de vitesse radiale (VR). Cela a permis la caractérisation de leur compagnons planétaires. J’ai analysé les spectres de 21 autres étoiles CoRoT et Kepler, probablement hôtes de naines M à faible masse. Cela a permis d’'élargir l'échantillon des étoiles à faible masse avec masse et rayon mesurés. J’ai calculé l’indice d’activité chromosphérique de 31 étoiles observées avec SOPHIE/OHP, en aidant l’étude des interactions étoile-planète. J’ai étudié le comportement de SOPHIE à bas signal à bruit (S/B). J’ai déterminé l’intervalle de S/B dans lequel un spectre stellaire est fiable pour la mesure des paramètres stellaires.Dans le cadre du consortium SOPHIE, j’ai suivi l’analyse complète du système Kepler-117. Ce système multi-planétaire montre variations des périodes orbitaux dues aux échanges dynamiques entre les planètes (TTV). Pour déterminer les paramètres du système, un approche spécifique a été développé pour l’ajustement simultané de transits, VR et TTV (Bruno et al. 2015).Finalement, je me suis intéressé à l’activité stellaire dans la photométrie de transit. J’ai impl ́ementé deux logiciels de modélisation de tâches stellaires dans un code MCMC, en ajoutant l’évolution des tâches dans l’un d’eux. J’ai appliqué les logiciels au Soleil, à CoRoT-7 et à CoRoT-2. J’ai amené un étude détaillé de la courbe de lumière de CoRoT-2, et exploré les effets des tâches dans les paramètres du transit (Bruno et al., en prep.). Avec la méthode FF’ (Aigrain et al. 2012), j’ai contribué à l’exploration du lien entre la signature des tâches de CoRoT-7 et dans la photométrie et dans les VR
During my PhD, I analyzed the spectra of nine Kepler stars obtained by radial velocity (RV) observations. This allowed the characterization of their planetary companions. I analyzed the spectra of twenty-one other CoRoT and Kepler stars, likely orbited by low-mass M dwarfs. This helped widening the sample of low-mass stars with measured mass and radius. I calculated the chromospheric activity indfex of thirty-one stars observed with SOPHIE/OHP, helping the study of star-planet interactions. I studied the behavior of SOPHIE in low signal-to-noise ratio (SNR) regime. I determinhed the SNR range in which a stellar spectrum is reliable for the measure of the stellar parameters.Within the SOPHIE consortium, I followed the complete analysis of the Kepler-117 system. This multi-planetary system presents variations in the planetary orbital periods due to their mutual dynamical interacion (TTVs). To fit the system parameters, a specific fitting approach including TTV modeling was developed. We derived the system parameters by the simultaneous fit of transits, RVs, and TTVs (Bruno et al. 2015).Finally, I addressed the problem of stellar activity in transit photometry. I implemented two starspot modeling codes into an MCMC algorithm, adding spot evolution to oneof them. I applied the codes to the Sun, CoRoT-7, and CoRoT-2. I carried an extensive study on the light curve of CoRoT-2, and explored the effects of the spots on the transit parameters (Bruno et al., in prep.). With the FF’ method (Aigrain et al. 2012), I contributed to explore the connection between the photometric and RV signature of starspots in CoRoT-7
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Fusillo, Nicola P. G. "Stellar and planetary remnants in large area surveys." Thesis, University of Warwick, 2015. http://wrap.warwick.ac.uk/77318/.

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The advent of large-area digital sky surveys marked a turning point for the entire field of astronomy. Today, with multi-band photometry for hundreds of millions of objects readily at hand, the ability to mine data for specific rare objects of interest has become of fundamental importance. The aim of this work was to study white dwarfs and planetary remnants by, first of all, developing efficient selection algorithms to identify these objects in large area surveys. Using SDSS DR7 we developed a routine which relies on colours and proper motion to calculate probabilities of being a white dwarf (PWD) which, in turn, enables a flexible selection of white dwarf candidates without recourse to spectroscopy. The application of this selection method to SDSS DR10 lead to the creation of a catalogue of ≃ 66, 000 bright (g ≤ 19) objects with calculated PWD from which it is possible to select ≃ 23, 000 high-confidence white dwarf candidates . The reliability of the method was further tested using a sample of spectroscopic objects from the LAMOST survey. This independent test confirmed the robustness of our algorithm and lead to the identification of 290 new white dwarfs. We also applied our selection routine to the recently released ATLAS DR2 to construct a preliminary catalogue of ≃ 9000 ATLAS white dwarf candidates. This catalogue represents the first sample of white dwarfs candidates in the southern hemisphere. We later exploited our catalogue in several science project. We developed a separate selection algorithm to identify variable white dwarfs in large area time-domain surveys. To test this method we carried out a pilot search for pulsating white dwarfs using 400 high-confidence white dwarfs candidates with available multi-epoch photometry in SDSS Stripe 82. This test proved the ability of our method to select different types of variable white dwarfs and allowed to identify 5 pulsating white dwarfs, 3 of which are new discoveries. During the development of our catalogue, we also identified 64 new metal polluted white dwarfs. Recent studies have shown that the metal pollution in these objects is the result of accretion of remnants of planetary systems. In a few cases these planetary remnants form a circustellar debris disc which can be detected as an infrared excess. Here we present the results of high-resolution spectroscopic follow-up of 15 of the newly identified metalpolluted white dwarfs. Using accurate spectral analyses of the atmospheres of these white dwarfs we determined chemical compositions and masses of the accreted bodies, and discuss the impact of these finding on the current knowledge of extra-solar planetary systems. Using optical and infrared photometric data from various large-area surveys we carried out a search for infrared excess around our newly identified metal polluted white dwarfs, and high-confidence white dwarf candidates. We identified four metal polluted white dwarfs with possible debris discs and compiled a list of ≃ 300 white dwarfs candidates with infrared excess ready for future spectroscopic follow-up.
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Girven, Jonathan. "Stellar and planetary remnants in digital sky surveys." Thesis, University of Warwick, 2012. http://wrap.warwick.ac.uk/53749/.

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Large scale digital sky surveys have produced an unprecedented volume of uniform data covering both vast proportions of the sky and a wide range of wavelength, from the ultraviolet to the near-infrared. The challenge facing astronomers today is how to use this multitude of information to extract trends, outliers and and rare objects. For example, a large sample of single white dwarf stars has the potential to probe the Galaxy through the luminosity function. The aim of this work was to study stellar and planetary remnants in these surveys. In the last few decades, it has been shown that a handful of white dwarfs have remnants of planetary systems around them, in the form of a dusty disc. These are currently providing the best constraints on the composition of extra-solar planetary systems. Finding significant numbers of dusty discs is only possible in large scale digital sky surveys. I ultilised the SDSS DR7 and colour-colour diagrams to and DA white dwarfs from optical photometry. This nearly doubled the number of spectroscopically con- armed DA white dwarfs in the SDSS compared with DR4 [Eisenstein et al., 2006], and introduced nearly 10; 000 photometric-only DA white dwarf candidates. I further cross-matched our white dwarf catalogue with UKIDSS LAS DR8 to carry out the currently largest and deepest untargeted search for low-mass companions to, and dust discs around, DA white dwarfs. Simultaneously, I analyzed Spitzer observations of 15 white dwarfs with metal-polluted atmospheres, all but one having helium-dominated atmospheres. Three of these stars were found to have an infrared excess consistent with a dusty disc. I used the total sample to estimate a typical disc lifetime of log[tdisc(yr)] = 5:6+1:1, which is compatible with the relatively large range estimated from different theoretical models. Subdwarf population synthesis models predicted a vast population of subdwarfs with F to K-type companions, produced in the effcient RLOF formation channel. I used a cross-match of ultraviolet, optical and infrared surveys to search for this unseen population. I select a complementary sample to those found from radial velocity surveys, offering direct tests of binary evolution pathways. Finally, I present a method to use common proper motion white dwarf pairs to constrain the initial-final mass relation, which is extremely uncertain at low masses. In the example I show, one of the stars is a magnetic white dwarf with B ' 6 MG, making this a rare and intriguing system from a magnetic white dwarf formation point of view.
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Savino, A. "On the complex stellar populations of ancient stellar systems." Thesis, Liverpool John Moores University, 2018. http://researchonline.ljmu.ac.uk/9190/.

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The study of ancient stellar systems in the vicinity of the Milky Way provides a wealth of information on the conditions, in the early Universe, that led to the properties we observe today in galaxies and in their constituent components. Resolved stellar populations enable us to gain detailed insights on the age and chemical composition of such stellar systems, tracing their properties on a fine spatial scale. The deep investigation of Local Group objects revealed that even very old, low mass, stellar systems host unexpected complexities in their stellar populations. Such complexities remain largely unexplained, our understanding limited by observational and theoretical limitations. Here I present work aimed at a deeper characterisation of the complex stellar popula- tions in dwarf spheroidal galaxies and Galactic globular clusters. I use a combination of observational and modelling techniques to shed light on the detailed stellar properties of these objects. Part of my investigation focuses on the horizontal branch of dwarf spheroidal galaxies. By careful modelling of the horizontal branch in the galaxy Carina, which has well known star formation history, I demonstrate that the horizontal branch contains precious information, that can be used to refine age measurements in nearby galaxies. To this aim, I develop a new modelling method that, for the first time, combines constraints from the main sequence turn-off and the horizontal branch to provide very precise measurements of the star formation history in resolved galaxies. The combined information from different regions of the colour-magnitude diagram permits to recover the value of mass loss experienced by red giant branch stars with very high precision. I test this technique on a range of synthetic populations and on the well studied galaxy Sculptor, demonstrating the increased age resolution that this approach provides. I apply my modelling tool to the distant galaxy Tucana, determining a very detailed star formation history, where multiple events of star formation can be clearly distinguished. The identification of the different stellar populations on the horizontal branch permits us to characterise the spatial distribution of the star formation events in this galaxy. I also perform a photometric study of the massive globular cluster M13, focussing on the multiple stellar populations present in this object. I identify and trace the different stellar populations out to most external regions of this cluster. The spatial distribution of these populations, which shows no sign of radial segregation, reveal the very advanced dynamical evolutionary stage of the cluster. The work presented in this manuscript constitutes a step forward to understand the formation of low mass ancient stellar systems and paves the way for deeper studies of large samples of stellar systems in the Milky Way vicinity.
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McLean, William George King. "Polarimetry of planetary systems." Thesis, University of Warwick, 2017. http://wrap.warwick.ac.uk/98039/.

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Light reflected by planetary atmospheres and/or surfaces is polarised, and the degree and direction of polarisation can yield information that cannot always be gleaned from flux measurements alone. Polarimetric studies of solar system planets can reveal more details about the seasonal variations in their atmospheres, and the variation with orbital geometry can place constraints on the properties of cloud particles. With the advent of extremely large telescopes, and potentially the most accurate instruments ever realised thus far, polarimetry has great potential for both detecting and characterising exoplanets. A key difference when observing exoplanets with respect to the planets of our solar system is that despite the much lower signal-to-noise than solar system planets, we can access them at wider phase angle ranges, thus enabling us to probe their scattering properties more extensively, especially at geometries where the degree of polarisation is highest. This can result in an easier interpretation of the atmospheric characteristics through theoretical modelling. My original contribution to the field that is presented in this thesis is the observation, data reduction and analysis of polarimetric data along with model interpretation of the six most outer solar system planets and Titan. In addition, model results for exoplanets of varying types are shown and discussed. The overall goal is to show that polarimetry is necessary for giving a full description of light reflected by planetary atmospheres and surfaces, and to demonstrate its worth as a diagnostic tool for atmospheric characterisation, from both ground-based observations of solar system and exoplanets, and from in-situ missions to the outer planets, such as a potential atmospheric probe into any of the outer planets.
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Nelson, Katy. "On the origin of the stellar initial mass function and multiple stellar systems." Thesis, Cardiff University, 2014. http://orca.cf.ac.uk/65971/.

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I first perform a statistical analysis on a distribution of pre-stellar core masses. Each core is split into a small number of stars, and two stars are chosen using a prescription based on stellar masses to form a binary system. The rest of the stars are taken to be singles. From this sample of binaries and singles, I compute the stellar initial mass function, the binary frequency and mass ratio distribution as a function of primary mass. I then test if the observed binary frequencies and mass ratios are compatible with this self-similar mapping of cores into stars. I show that self-similar mapping can reproduce the observed binary frequencies and mass ratios well, so long as the efficiency is rather high (100%), and each core fragments into about 4 or 5 stars. Using the code Seren view, I then perform N-body simulations with core-clusters. I investigate the formation of multiple systems, and qualify the dependence of their parameters and longevity on certain initial conditions, including (i) the number of stars in a core-cluster, (ii) the variance of masses in those stars, (iii) the virial ratio and (iv) radial dependence of stellar density. I expand on those results by including (a) a prescription for the influence of disks during stellar ybys, (b) different initial spatial configurations of the stars (i.e. line and ring clusters) and (c) a background potential due to residual gas in the core-cluster. The full range of periods observed in the field cannot be explained by the distribution of periods of pure binaries alone, which is too narrow. However, the wide range can be explained either by combining the periods of pair-wise orbits of all multiple systems, i.e. the widest periods observed are in fact pair-wise orbits of higher-order multiples with unresolved companions, or by considering a distribution of pre-stellar cores that have a range of virial ratios.
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Skemer, Andrew. "HIGH SPATIAL RESOLUTION MID-INFRARED STUDIES OF PLANETARY SYSTEMS." Diss., The University of Arizona, 2011. http://hdl.handle.net/10150/202978.

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I present the results of six papers related the formation and evolution of planets and planetary systems, all of which are based on high-resolution, ground-based, mid-infrared observations.The first three chapters are studies of T Tauri binaries. T Tauri stars are young, low mass stars, whose disks form the building blocks of extrasolar planets. The first chapter is a study of the 0.68"/0.12" triple system, T Tauri. Our spatially resolved N-band photometry reveals silicate absorption towards one component, T Tau Sa, indicating the presence of an edge-on disk, which is in contrast to the other components. The second chapter is an adaptive optics fed N-band spectroscopy study of the 0.88" binary, UY Aur. We find that the dust grains around UY Aur A are ISM-like, while the mineralogy of the dust around UY Aur B is more uncertain, due to self-extinction. The third chapter presents a survey of spatially resolved silicate spectroscopy for nine T Tauri binaries. We find with 90\%-95\% confidence that the silicate features of the binaries are more similar than those of randomly paired single stars. This implies that a shared binary property, such as age or composition, is an important parameter in dust grain evolution.The fourth chapter is a study of the planetary system, 2MASS 1207. We explore the source of 2MASS 1207 b's under-luminosity, which has typically been explained as the result of an edge-on disk of large, grey-extincting dust grains. We find that the edge-on disk theory is incompatible with several lines of evidence, and suggest that 2MASS 1207 b's appearance can be explained by a thick cloudy atmosphere, which might be typical among young, planetary systems.The fifth chapter is a study of the white dwarf, Sirius B, which in the context of this thesis is being studied as a post-planetary system. Our N-band imaging demonstrates that Sirius B does not have an infrared excess, in contrast to previous results.The sixth chapter is a study of mid-infrared atmospheric dispersion, which in the context of this thesis is being studied as an effect that will limit the ability of ELTs to image planetary systems. We measure mid-infrared atmospheric dispersion, for the first time, and use our results to confirm theoretical models.
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Books on the topic "Stellar astronomy and planetary systems"

1

Oswalt, Terry D. Planets, Stars and Stellar Systems: Volume 3: Solar and Stellar Planetary Systems. Dordrecht: Springer Netherlands, 2013.

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Oswalt, Terry D. Planets, Stars and Stellar Systems: Extragalactic Astronomy and Cosmology. Dordrecht: Springer Netherlands, 2013.

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Jacobsen, Theodor S. Planetary systems from the ancient Greeks to Kepler. [Seattle]: Dept. of Astronomy, University of Washington, in association with the University of Washington Press, 1999.

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Ollivier, Marc. Planetary Systems: Detection, formation and habitability of extrasolar planets. Edited by Encrenaz Thérèse, Trimble V, Selsis Franck, Roques Francoise, Maeder A, Lequeux J, Grebel E. K, et al. Berlin, Heidelberg: Springer-Verlag, 2010.

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1953-, Weaver Harold A., Danly L, and Space Telescope Science Institute (U.S.), eds. 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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D, Monnier John, Schöller Markus, Danchi William Clifford, American Astronomical Society, and Society of Photo-optical Instrumentation Engineers., eds. Advances in stellar interferometry: 25-30 May 2006, Orlando, Florida, USA. Bellingham, Wash: SPIE, 2006.

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National Research Council (U.S.). Committee on Planetary and Lunar Exploration. Strategy for the detection and study of other planetary systems and extrasolar planetary materials, 1990-2000. Washington, D.C: National Academy Press, 1990.

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Anthony, Young. Lunar and planetary rovers: The wheels of Apollo and the quest for Mars. New York ; Berlin: Springer, 2007.

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G, Byrd Gene, ed. Order and chaos in stellar and planetary systems: Proceedings of a meeting held in Saint Petersburg, Russia, 17-24 August 2003. San Francisco, Calif: Astronomical Society of the Pacific, 2004.

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Stern, S. Alan. A semi-annual report for studies of extra-solar Oort Clouds and the Kuiper Disk. San Antonio, Texas: Southwest Research Institute, Instrumentation and Space Research Division, 1993.

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Book chapters on the topic "Stellar astronomy and planetary systems"

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Basu, Shantanu, and Pranav Sharma. "Stellar and Planetary Systems." In Essential Astrophysics, 115–32. Boca Raton: CRC Press, 2021. http://dx.doi.org/10.1201/9781003215943-6.

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Moro-Martın, Amaya. "Dusty Planetary Systems." In Planets, Stars and Stellar Systems, 431–87. Dordrecht: Springer Netherlands, 2013. http://dx.doi.org/10.1007/978-94-007-5606-9_9.

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Bagenal, Fran. "Planetary Magnetospheres." In Planets, Stars and Stellar Systems, 251–307. Dordrecht: Springer Netherlands, 2013. http://dx.doi.org/10.1007/978-94-007-5606-9_6.

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Tiscareno, Matthew S. "Planetary Rings." In Planets, Stars and Stellar Systems, 309–75. Dordrecht: Springer Netherlands, 2013. http://dx.doi.org/10.1007/978-94-007-5606-9_7.

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von Braun, Kaspar, and Tabetha Boyajian. "The Determination of Stellar and Planetary Astrophysical Parameters." In SpringerBriefs in Astronomy, 5–21. Cham: Springer International Publishing, 2017. http://dx.doi.org/10.1007/978-3-319-61198-3_2.

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Artymowicz, Pawel. "Planetary Systems." In Impact of Modern Dynamics in Astronomy, 313–16. Dordrecht: Springer Netherlands, 1999. http://dx.doi.org/10.1007/978-94-011-4527-5_31.

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Vázquez, M., E. Pallé, and P. Montañés Rodríguez. "Extrasolar Planetary Systems." In Astronomy and Astrophysics Library, 337–90. New York, NY: Springer New York, 2010. http://dx.doi.org/10.1007/978-1-4419-1684-6_8.

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Encrenaz, Thérèse, Jean-Pierre Bibring, Michel Blanc, Maria-Antonietta Barucci, Francoise Roques, and Philippe Zarka. "New Planetary Systems." In Astronomy and Astrophysics Library, 463–85. Berlin, Heidelberg: Springer Berlin Heidelberg, 2004. http://dx.doi.org/10.1007/978-3-662-10403-3_14.

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Schröder, Klaus-Peter, Hilmar W. Duerbeck, and Johannes Viktor Feitzinger. "Stars and Stellar Systems." In Handbook of Practical Astronomy, 573–695. Berlin, Heidelberg: Springer Berlin Heidelberg, 2009. http://dx.doi.org/10.1007/978-3-540-76379-6_14.

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Tokunaga, Alan T., William D. Vacca, and Erick T. YoungDr. "Infrared Astronomy Fundamentals." In Planets, Stars and Stellar Systems, 99–174. Dordrecht: Springer Netherlands, 2013. http://dx.doi.org/10.1007/978-94-007-5618-2_3.

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Conference papers on the topic "Stellar astronomy and planetary systems"

1

Marov, M. Ya, and 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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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.
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Konovalenko, A. A. "New Antennas and Methods for the Low Frequency Stellar and Planetary Radio Astronomy." In Planetary Radio Emissions VII. Vienna: Austrian Academy of Sciences Press, 2011. http://dx.doi.org/10.1553/pre7s521.

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Artymowicz, Pawel. "Planetary Systems." In GRADUATE SCHOOL IN ASTRONOMY: X Special Courses at the National Observatory of Rio de Janeiro (X CCE). AIP, 2006. http://dx.doi.org/10.1063/1.2219324.

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Mumma, Michael J. "Planetary astronomy in the 21st century—The study of planetary systems." In Astrophysics from the Moon. AIP, 1990. http://dx.doi.org/10.1063/1.39347.

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Skemer, Andrew J., R. Deno Stelter, Dimitri Mawet, Michael P. Fitzgerald, Benjamin A. Mazin, Olivier Guyon, Christian Marois, et al. "The planetary systems imager: 2-5 micron channel." In Ground-based and Airborne Instrumentation for Astronomy VII, edited by Hideki Takami, Christopher J. Evans, and Luc Simard. SPIE, 2018. http://dx.doi.org/10.1117/12.2314173.

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Fitzgerald, Michael P., Stephanie Sallum, Maxwell Millar-Blanchaer, Rebecca Jensen-Clem, Philip Hinz, Olivier Guyon, Jason Wang, et al. "The Planetary Systems Imager for TMT: overview and status." In Ground-based and Airborne Instrumentation for Astronomy IX, edited by Christopher J. Evans, Julia J. Bryant, and Kentaro Motohara. SPIE, 2022. http://dx.doi.org/10.1117/12.2630410.

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Kim, Hyosun, and Ronald E. Taam. "The Interaction of Planets and Brown Dwarfs with AGB Stellar Winds." In PLANETARY SYSTEMS BEYOND THE MAIN SEQUENCE: Proceedings of the International Conference. AIP, 2011. http://dx.doi.org/10.1063/1.3556184.

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Béjar, V. J. S., M. R. Zapatero Osorio, A. Pérez-Garrido, C. Álvarez, E. L. Martín, R. Rebolo, I. Villó-Pérez, A. Díaz-Sánchez, and Eric Stempels. "Discovery of a wide planetary-mass companion of a brown dwarf in the Upper Scorpius association." In COOL STARS, STELLAR SYSTEMS AND THE SUN: Proceedings of the 15th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun. AIP, 2009. http://dx.doi.org/10.1063/1.3099150.

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Sallum, Stephanie, Michael P. Fitzgerald, Maxwell Millar-Blanchaer, Jason Wang, Rebecca Jensen-Clem, and Andy Skemer. "The Planetary Systems Imager: driving science cases and top level requirements." In Ground-based and Airborne Instrumentation for Astronomy IX, edited by Christopher J. Evans, Julia J. Bryant, and Kentaro Motohara. SPIE, 2022. http://dx.doi.org/10.1117/12.2630423.

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Madappatt, Niyas, Orsola De Marco, Jason Nordhaus, and Mark Wardle. "Towards a New Prescription for the Tidal Capture of Planets, Brown Dwarfs and Stellar Companions." In PLANETARY SYSTEMS BEYOND THE MAIN SEQUENCE: Proceedings of the International Conference. AIP, 2011. http://dx.doi.org/10.1063/1.3556219.

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