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Dissertations / Theses on the topic 'Formation and evolution of planetary systems'

Author: Grafiati

Published: 8 June 2024

Last updated: 31 July 2025

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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.<br>Cataloged from PDF version of thesis.<br>Includes bibliographical references (pages 299-311).<br>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

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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 ho

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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

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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

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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.

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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 comp

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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.

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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.<br>Earth and Planetary Sciences

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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.<br>Vita.<br>Includes bibliographical references.<br>by David Speir McCormick.<br>Ph.D.

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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 (fragmentat

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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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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 simul

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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.<br>Includes bibliographical references (p. 159-170).<br>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 engi

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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 characterisi

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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.

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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<br>Cataloged from PDF of thesis.<br>Includes bibliographical references (pages 151-174).<br>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

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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, howeve

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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 protop

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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 Ob

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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

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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 s

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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.<br>Cataloged from PDF version of thesis.<br>Includes bibliographical references (pages 104-115).<br>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 thro

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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

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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 s

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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

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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

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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 p

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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 km<sup>2</sup> 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 stor

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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<br>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 bas

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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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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 o

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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 accor

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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

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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 maré

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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 nai

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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 interféromètr

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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

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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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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 avo

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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

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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.<br>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 co

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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 f

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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 distan

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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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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 confi

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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

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"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_s

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