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Dissertations / Theses on the topic 'Planets'

Author: Grafiati

Published: 4 June 2021

Last updated: 25 July 2025

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1

Brickman, Jacklyn E. "Experiments in Biological Planet Formation and Plants: Nourishing Bodies, Nourishing Planets." The Ohio State University, 2020. http://rave.ohiolink.edu/etdc/view?acc_num=osu1595340630648528.

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2

Trotta, Leonardo Di Schiavi. "Modelo dinâmico 3-D para a evolução do sistema Plutão-Caronte /." Rio Claro, 2017. http://hdl.handle.net/11449/150604.

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Orientador: Tadashi Yokoyama<br>Banca: Nelson Callegari Junior<br>Banca: Rodney da Silva Gomes<br>Resumo: O sistema Plutão-Caronte é um par quase binário em estado de duplo sincronismo. Hoje sabe-se que Plutão possui cinco satélites: Caronte, Styx, Nix, Kerberos e Hydra, onde os últimos quatro são muito menores que Caronte. A origem mais plausível para o sistema Plutão-Caronte é a de um impacto de grandes proporções entre corpos de tamanhos similares, onde o impactador (que viria a ser Caronte) permanece quase intacto após o evento. Caronte iniciaria o movimento orbital próximo de Plutão (ex:

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3

Joos, Franco. "Polarimetry of gas planets /." Zürich : ETH, 2007. http://e-collection.ethbib.ethz.ch/show?type=diss&nr=17051.

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4

Turner, Jake D., Robin M. Leiter, Lauren I. Biddle, et al. "Investigating the physical properties of transiting hot Jupiters with the 1.5-m Kuiper Telescope." OXFORD UNIV PRESS, 2017. http://hdl.handle.net/10150/626279.

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We present new photometric data of 11 hot Jupiter transiting exoplanets (CoRoT-12b, HATP-5b, HAT-P-12b, HAT-P-33b, HAT-P-37b, WASP-2b, WASP-24b, WASP-60b, WASP-80b, WASP-103b and XO-3b) in order to update their planetary parameters and to constrain information about their atmospheres. These observations of CoRoT-12b, HAT-P-37b and WASP-60b are the first follow-up data since their discovery. Additionally, the first near-UV transits of WASP-80b and WASP-103b are presented. We compare the results of our analysis with previous work to search for transit timing variations (TTVs) and a wavelength de

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5

Ortiz, Álvarez Mauricio [Verfasser], and Andreas [Akademischer Betreuer] Quirrenbach. "Planets around giant stars: Two close-in transiting planets and one S-type planet in an eccentric binary system / Mauricio Ortiz Álvarez ; Betreuer: Andreas Quirrenbach." Heidelberg : Universitätsbibliothek Heidelberg, 2017. http://d-nb.info/118073890X/34.

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6

Lines, Stefan Matthew. "The formation of circumbinary planets." Thesis, University of Bristol, 2016. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.702118.

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The discovery of nearly two thousand extrasolar planets over the last two decades is indicative that planets form everywhere. Exoplanet detections have been made of a plethora of planetary types and sizes across a wide range of orbital characteristics. One of the more exotic locations that planets have been discovered in is around stellar binaries. Their proximity to such a large time-dependent potential from the orbital motion of the stars can be problematic for their formation and long-term stability. Circumbinary planets, with orbits that fully encompass the binary, have been found to orbit

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7

Janes, Daniel Mark. "Tectonics of one-plate planets." Diss., The University of Arizona, 1990. http://hdl.handle.net/10150/185087.

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The Voyager 2 encounter with Neptune and its moons in August of 1989 completed the discovery phase of planetary exploration. In the 25 years since Mariner 4 returned the first images of another planet, geophysical models for such basic processes as mantle convection and loading which were developed for the Earth have been strained beyond their limits by features such as the Tharsis rise on Mars and the coronae of Miranda which cover as much as a quarter of their planetary circumference. In this work I develop a general planetary shell model in spherical coordinates that is capable of treating

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8

Fortney, Jonathan J. "The evolution of giant planets." Diss., The University of Arizona, 2004. http://hdl.handle.net/10150/290002.

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As a whole this dissertation aims to understand giant planets as an entire class of astronomical objects. Initially we investigate the mechanics and evolutionary effects of phase separation in the deep interiors of giant planets. We present the first models of Saturn and Jupiter to couple their evolution to both a radiative-atmosphere grid and to high-pressure phase diagrams of hydrogen with helium and other admixtures. We find that previously calculated hydrogen-helium phase diagrams in which Saturn's interior reaches a region of predicted helium immiscibility do not allow enough energy relea

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9

Zaranek, Sarah Ellen. "Roles of convection in the evolution of planetary interiors and terrestrial lithospheres /." View online version; access limited to Brown University users, 2005. http://wwwlib.umi.com/dissertations/fullcit/3174708.

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10

Steffen, Jason. "Detecting new planets in transiting systems /." Thesis, Connect to this title online; UW restricted, 2006. http://hdl.handle.net/1773/9686.

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11

Barker, Adrian John. "Tidal interactions between planets and stars." Thesis, University of Cambridge, 2011. https://www.repository.cam.ac.uk/handle/1810/240581.

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Since the first discovery of an extrasolar planet around a solar-type star, observers have detected over 500 planets outside the solar system. Many of these planets have Jovian masses and orbit their host stars in orbits of only a few days, the so-called 'Hot Jupiters'. At such close proximity to their parent stars, strong tidal interactions between the two bodies are expected to cause significant secular spin-orbit evolution. This thesis tackles two problems regarding the tidal evolution of short-period extrasolar planets. In the first part, we adopt a simple model of the orbit-averaged effec

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12

Carter, Andrew James. "Observation and modeling of extrasolar planets." Thesis, Open University, 2011. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.578669.

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The field of exoplanet research has currently yielded the discovery of 552 planets. This figure includes 132 transiting planets which can be studied in greater detail and have formed the cornerstone of research to characterise the exoplanet population. In particular, such studies seek to analyse the planetary atmospheres, but research has thus far yielded more questions than answers. Exoplanetary atmospheric studies have typically focussed on one planet apiece - complicating any comparative analysis as every result employs different methods and instruments. For a comprehensive, comparative stu

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13

Tsapras, Yiannis. "Microlensing search for extra solar planets." Thesis, University of St Andrews, 2002. http://hdl.handle.net/10023/7092.

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Gravitational microlensing may be used to probe distant stars for planetary companions. The presence of a planet in the vicinity of a star acting as the lens may cause a short lived anomaly in the observed lightcurve of the lensing event. By quantifying these anomalies we may place limits on the mass of the companion relative to the lens as well as the position of the planet relative to the primary lens. The detection probability is proportional to mp, where mp is the planet mass. All current follow-up teams use dedicated observations on a preselected sample of mainly high-amplification events

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14

Watkins, Christopher Lloyd. "Atmospheric gravity waves on giant planets." Thesis, Queen Mary, University of London, 2012. http://qmro.qmul.ac.uk/xmlui/handle/123456789/8683.

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Internal gravity waves are a common feature of stratified fluids. They facilitate transport of momentum and energy – thus influencing the evolution of the fluid. There is a large body of research addressing the behaviour of gravity waves in the terrestrial atmosphere. This thesis builds and extends the research to giant planets – in particular to close-in extrasolar giant planets and the solar system giant planet, Jupiter. Because the atmospheres of close-in giant planets are expected to be strongly stratified, knowledge of the behaviour of gravity waves in such atmospheres is especially impor

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15

Muterspaugh, Matthew Ward. "Binary star systems and extrasolar planets." Thesis, Massachusetts Institute of Technology, 2005. http://hdl.handle.net/1721.1/34646.

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Thesis (Ph. D.)--Massachusetts Institute of Technology, Dept. of Physics, 2005.<br>Includes bibliographical references (p. 121-137).<br>For ten years, planets around stars similar to the Sun have been discovered, confirmed, and their properties studied. Planets have been found in a variety of environments previously thought impossible. The results have revolutionized the way in which scientists understand planet and star formation and evolution, and provide context for the roles of the Earth and our own solar system. Over half of star systems contain more than one stellar component. Despite th

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16

Mustill, Alexander James. "The dynamics of planets and discs." Thesis, University of Cambridge, 2012. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.610345.

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17

Jackson, Brian. "Tidal Evolution of Extra-Solar Planets." Diss., The University of Arizona, 2009. http://hdl.handle.net/10150/196152.

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In both our solar system and extra-solar planetary systems, tides may have a variety of effects, driving complex orbital evolution and geophysical processes. For extra-solar planets with orbits that pass very close to their host stars, tides have reduced orbital eccentricities and semi-major axes, and the rates of tidal evolution may change dramatically as orbits evolve. Understanding how the orbits have evolved and, ultimately, discerning the origins of close-in extra-solar planets require accounting for all the complexity of tidal evolution. The accompanying dissipation of tidal energy withi

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18

Loyd, R. O. Parke, T. T. Koskinen, Kevin France, Christian Schneider, and Seth Redfield. "Ultraviolet C ii and Si iii Transit Spectroscopy and Modeling of the Evaporating Atmosphere of GJ436b." IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/624389.

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Hydrogen gas evaporating from the atmosphere of the hot-Neptune GJ436b absorbs over 50% of the stellar Lya emission during transit. Given the planet's atmospheric composition and energy-limited escape rate, this hydrogen outflow is expected to entrain heavier atoms such as C and O. We searched for C and Si in the escaping atmosphere of GJ436b using far-ultraviolet Hubble Space Telescope COS G130M observations made during the planet's extended H I transit. These observations show no transit absorption in the C II 1334,1335 angstrom and Si III 1206 angstrom lines integrated over [-100, 100] km s

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19

Turner, Oliver David. "Discovery and characterisation of transiting extra-solar planets with the Wide Angle Search for Planets (WASP) survey." Thesis, Keele University, 2017. http://eprints.keele.ac.uk/3563/.

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In July of 2012 the WASP-South instrument was modified to allow it to collect data on brighter stars. This change was motivated by the dearth of planets known to orbit bright hosts in the southern hemisphere and the depth of study possible for HD209458 b and HD189733 b. These two planets orbit very bright stars in the northern hemisphere and have lead to a wealth of discoveries thanks to the relative ease with which they can be studied. My initial work with the Wide Angle Search for Planets (WASP) project was to contribute to updating the existing automated data reduction pipeline. I investiga

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20

McLeod, Scott Stuart. "Isostatically compensated extensional tectonics on Enceladus." Thesis, Montana State University, 2009. http://etd.lib.montana.edu/etd/2009/mcleod/McLeodS0509.pdf.

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Saturn's moon Enceladus is the smallest body in the solar system known to be geologically active. Extensive, energetic resurfacing processes are ongoing and it possesses a system of geysers at the South Pole that supply material to the E-ring. The South Polar Terrain (SPT) is the youngest region on Enceladus and its contacts with the older cratered and grooved plains to the north are delineated by a variety of complex geologic features including mountain ranges and massive grabens. Many of the geologic features seen on Enceladus bear superficial resemblance to terrestrial structures associated

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21

Turse, Carol Louise. "Testing the hydrogen peroxide-water hypothesis of life on Mars using the differential scanning calorimeter as an analog for the TEGA instrument on the Mars Phoenix lander." Pullman, Wash. : Washington State University, 2009. http://www.dissertations.wsu.edu/Thesis/Summer2009/c_turse_072309.pdf.

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Thesis (M.S. in environmental science)--Washington State University, August 2009.<br>Title from PDF title page (viewed on Sept. 22, 2009). "School of Earth and Environmental Sciences." Includes bibliographical references (p. 92-97).

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22

Underwood, David R. "The stability of orbits of putative Earth-mass planets or satellites of giant planets within known exoplanetary systems." Thesis, Open University, 2006. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.437779.

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23

Espinoza, Nestor, Rafael Brahm, Andres Jordan, et al. "DISCOVERY AND VALIDATION OF A HIGH-DENSITY SUB-NEPTUNE FROM THE K2 MISSION." IOP PUBLISHING LTD, 2016. http://hdl.handle.net/10150/624071.

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We report the discovery of K2-56b, a high-density sub-Neptune exoplanet, made using photometry from Campaign 4 of the two-wheeled Kepler (K2) mission, ground-based radial velocity (RV) follow-up from HARPS and high-resolution lucky and adaptive optics imaging obtained using AstraLux and MagAO, respectively. The host star is a bright (V - 11.04, K-s - 9.37), slightly metal-poor ([Fe/H] - -0.15 +/- 0.05 dex) solar analogue located at 152.1(-7.4)(+9.7) pc from Earth, for which we find a radius of R-* = 0.928(-04040)(+0.055) and a mass of M-* = 0.961(-0.029)(+0.032) M-circle dot. A joint analysis

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24

Doellinger, Michaela. "Hunting for extrasolar planets around K giants." Diss., lmu, 2008. http://nbn-resolving.de/urn:nbn:de:bvb:19-99700.

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25

Leigh, Christopher. "The detection and characterisation of extrasolar planets." Thesis, University of St Andrews, 2004. http://hdl.handle.net/10023/12943.

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Since the discovery of 51 Pegasi b in 1995, continued observations have indirectly identified over 110 planetary objects. These Jupiter-mass objects cause their host star to "wobble" slightly about the common centre-of-mass of the system, which is detectable as radial motion in high-precision Doppler spectroscopy. Of the known planets, approximately 20% are found to orbit within 0.1 AU of the star, whilst the transit of HD209458 has inferred the gas-giant nature of these close-in extrasolar giant planets (CEGPs). The discovery of CEGPs has produced a wave of speculative theory as to the exact

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26

Joiner, Joanna. "Millimeter-wave spectra of the jovian planets." Diss., Georgia Institute of Technology, 1991. http://hdl.handle.net/1853/15641.

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27

Barnett, D. N. "Convection, elasticity and flexure inside terrestrial planets." Thesis, University of Cambridge, 2001. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.596394.

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In this dissertation, the large-scale geophysical behaviour of the Earth, Venus and Mars are compared, using data collected by the Magellan spaceprobe (for Venus) and the Viking and Mars Global Surveyor (MGS) probes (for Mars). Neither Venus nor Mars show evidence of plate tectonics operating at the present day. On Venus, the lack of water means the frictional resistance at faults and the viscous drag on the base of the moving lithospheric plates are too high to be overcome by the driving forces for plate tectonics. The high elastic thickness of Mars results in a large frictional resistance to

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Lam, Hoanh An. "H'+â†3 in the jovian planets." Thesis, University College London (University of London), 1996. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.338995.

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29

Daley-Yates, Simon. "Radio emission from hot stars and planets." Thesis, University of Birmingham, 2018. http://etheses.bham.ac.uk//id/eprint/8585/.

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The winds of hot massive stars and hot giant planets grant us insight into the mechanisms by which the interstellar medium is enriched and the history behind planetary system formation. This thesis comprises a series of studies investigating the magnetospheric dynamics and emission properties of both these astronomical bodies. An analytic study of thermal radio and sub-mm emission from the winds of massive stars investigates the contribution from acceleration and wind clumping. The results show strong variation of the spectral index, corresponding to the wind acceleration region and clumping o

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Nikku, Madhusudhan 1980. "Retrieval of atmospheric properties of extrasolar planets." Thesis, Massachusetts Institute of Technology, 2009. http://hdl.handle.net/1721.1/63006.

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Thesis (Ph. D.)--Massachusetts Institute of Technology, Dept. of Physics, 2009.<br>Cataloged from PDF version of thesis.<br>Includes bibliographical references (p. 133-137).<br>We present a new method to retrieve molecular abundances and temperature profiles from exoplanet atmosphere photometry and spectroscopy. Our method allows us to run millions of 1-D atmosphere models in order to cover the large range of allowed parameter space. In order to run such a large number of models, we have developed a parametric pressure-temperature (P-T) profile coupled with line-by-line radiative transfer, hyd

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Verrier, Patricia Eleanor. "The dynamics of planets in multistellar systems." Thesis, University of Cambridge, 2008. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.612466.

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32

Kipping, D. M. "The transits of extrasolar planets with moons." Thesis, University College London (University of London), 2011. http://discovery.ucl.ac.uk/1306758/.

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The search for extrasolar planets is strongly motivated by the goal of characterizing how frequent habitable worlds and life may be within the Galaxy. Whilst much effort has been spent on searching for Earth-like planets, large moons may also be common, temperate abodes for life as well. The methods to detect extrasolar moons, or “exomoons” are more subtle than their planetary counterparts and in this thesis I aim to provide a method to find such bodies in transiting systems, which offer the greatest potential for detection. Before one can search for the tiny perturbations to the planetary sig

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33

Hoyer, Miranda Sergio David. "Search for unseen planets transit timing variations." Tesis, Universidad de Chile, 2012. http://www.repositorio.uchile.cl/handle/2250/111555.

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Doctor en Ciencias, Mención Astronomía<br>Observing the changes in the orbital period of transiting exoplanets produced by gravitational perturbations allows to detect unseen orbital companions in the system. With this technique,known asTransitTimingVariations(TTVs),itispossibletodetectperturbers down to Earth-like masses, overcoming the limits of current Radial Velocity searches. This PhDthesishasled to along termproject: TransitMonitoringin theSouth(TraMoS)project, which consists in a methodical and homogeneous monitoring of transiting exoplanets observable from the Southern Hemisphere with

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Jermyn, Adam Sean. "Turbulence and transport in stars and planets." Thesis, University of Cambridge, 2018. https://www.repository.cam.ac.uk/handle/1810/278021.

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In this dissertation I have argued that the study of stars and gaseous planets has relied too heavily on simplifying assumptions. In particular, I have demonstrated that the assumptions of spherical symmetry, thermal equilibrium, dynamical equilibrium and turbulent anisotropy all hide interesting phenomena which make a true difference to the structure and evolution of these bodies. To begin I developed new theoretical tools for probing these phenomena, starting with a new model of turbulent motion which accounts for many different sources of anisotropy. Building on this I studied rotating conv

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35

Portron, Stéphane. "Epicyclic gears dynamics and planets support conditions." Thesis, Lyon, 2019. http://www.theses.fr/2019LYSEI061.

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Ce doctorat est issu d'un partenariat entre SAFRAN Transmission Systems et le laboratoire LaMCoS de l'INSA de Lyon et dans le cadre la chaire INSA-SAFRAN "Transmissions mécaniques innovantes pour l'aéronautique". L'introduction de trains planétaires dans les turbofans a récemment émergé comme une solution technologique prometteuse pour réduire la vitesse de rotation des aubes dans la prochaine génération de moteurs d'avions. Au vu des vitesses de rotation et des charges au cours du fonctionnement, les paliers hydrodynamiques apparaissent comme une solution intéressante puisque d'une part ils p

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36

Gaudi, B. Scott. "Microlensing and the search for extrasolar planets /." The Ohio State University, 2000. http://rave.ohiolink.edu/etdc/view?acc_num=osu1488199501405399.

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37

Dressing, Courtney Danielle. "The Prevalence and Compositions of Small Planets." Thesis, Harvard University, 2015. http://nrs.harvard.edu/urn-3:HUL.InstRepos:17467474.

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This thesis describes three investigations of the galactic abundance and properties of small planets. First, I revised the properties of the smallest Kepler target stars and searched their light curves for transits using a custom transit detection pipeline. Combining the detected population of 156 planet candidates (including one previously undetected candidate) with an empirical estimate of the search completeness based on transit injection and recovery simulations, I found occurrence rates of 0.24 (+0.18/-0.08) Earth-size planets (1− 1.5 Earth radii) and 0.21 (+0.11/-0.06) super-Earths (1.5

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38

Langton, Jonathan. "Atmospheric dynamics on strongly irradiated Jovian planets /." Diss., Digital Dissertations Database. Restricted to UC campuses, 2008. http://uclibs.org/PID/11984.

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39

Lewis, Nikole Kae. "Atmospheric Circulation of Eccentric Extrasolar Giant Planets." Diss., The University of Arizona, 2012. http://hdl.handle.net/10150/242352.

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This dissertation explores the three-dimensional coupling between radiative and dynamical processes in the atmospheres of eccentric extrasolar giant planets GJ436b, HAT-P-2b, and HD80606b. Extrasolar planets on eccentric orbits are subject to time-variable heating and probable non-synchronous rotation, which results in significant variations in global circulation and thermal patterns as a function of orbital phase. Atmospheric simulations for the low eccentricity (e=0.15) Neptune sized planet GJ436b reveal that when Neptune-like atmospheric compositions are assumed day/night temperature co

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Moro-Martin, Maria A. "Signatures of planets in circumstellar debris disks." Diss., The University of Arizona, 2004. http://hdl.handle.net/10150/290124.

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Main sequence stars are commonly surrounded by debris disks, composed of cold dust continuously replenished by a reservoir of undetected dust-producing planetesimals. In the outer Solar System, Kuiper Belt (KB) objects produce dust by mutual or interstellar grain collisions. The orbital evolution of KB dust has been numerically modeled. Its equilibrium radial density distribution can be accurately estimated even though there are inherent uncertainties in the prediction of structure, owing to the chaotic dynamics of dust orbital evolution imposed by resonant gravitational perturbations of the p

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Sissa, Elena. "Observation of extrasolar planets at various ages." Doctoral thesis, Università degli studi di Padova, 2017. http://hdl.handle.net/11577/3426311.

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The search and characterization of extrasolar planets is one of the main topics of current astronomy, with the ultimate goals of understanding the formation and evolution of planetary systems, the general conditions for the formation of life-friendly environments, and possibly detecting signature of extra-solar life. In the last decades the research of extrasolar planets underwent a steep increase of interest and different methods of detection were developed. Each of them has its own merit and lack in studying the extrasolar system architecture and the characteristics of extrasolar planets.

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Wahl, Sean M., William B. Hubbard, and Burkhard Militzer. "TIDAL RESPONSE OF PRELIMINARY JUPITER MODEL." IOP PUBLISHING LTD, 2016. http://hdl.handle.net/10150/622055.

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In anticipation of improved observational data for Jupiter's gravitational field, from the Juno spacecraft, we predict the static tidal response for a variety of Jupiter interior models based on ab initio computer simulations of hydrogen-helium mixtures. We calculate hydrostatic-equilibrium gravity terms, using the non-perturbative concentric Maclaurin Spheroid method that eliminates lengthy expansions used in the theory of figures. Our method captures terms arising from the coupled tidal and rotational perturbations, which we find to be important for a rapidly rotating planet like Jupiter. Ou

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Komacek, Thaddeus D., and Dorian S. Abbot. "EFFECT OF SURFACE-MANTLE WATER EXCHANGE PARAMETERIZATIONS ON EXOPLANET OCEAN DEPTHS." IOP PUBLISHING LTD, 2016. http://hdl.handle.net/10150/622455.

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Terrestrial exoplanets in the canonical habitable zone may have a variety of initial water fractions due to random volatile delivery by planetesimals. If the total planetary water complement is high, the entire surface may be covered in water, forming a "waterworld." On a planet with active tectonics, competing mechanisms act to regulate the abundance of water on the surface by determining the partitioning of water between interior and surface. Here we explore how the incorporation of different mechanisms for the degassing and regassing of water changes the volatile evolution of a planet. For

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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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Tan, Xianyu, and Adam P. Showman. "Effects of Latent Heating on Atmospheres of Brown Dwarfs and Directly Imaged Planets." IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/624643.

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The growing number of observations of brown dwarfs (BDs) has provided evidence for strong atmospheric circulation on these objects. Directly imaged planets share similar observations and can be viewed as low-gravity versions of BDs. Vigorous condensate cycles of chemical species in their atmospheres are inferred by observations and theoretical studies, and latent heating associated with condensation is expected to be important in shaping atmospheric circulation and influencing cloud patchiness. We present a qualitative description of the mechanisms by which condensational latent heating influe

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Costa, André Izidoro Ferreira da [UNESP]. "Estudos da formação de planetas terrestres." Universidade Estadual Paulista (UNESP), 2013. http://hdl.handle.net/11449/102493.

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Made available in DSpace on 2014-06-11T19:32:09Z (GMT). No. of bitstreams: 0 Previous issue date: 2013-03-06Bitstream added on 2014-06-13T21:03:28Z : No. of bitstreams: 1 costa_aif_dr_guara.pdf: 4600583 bytes, checksum: 3d77d0ac5008ebea1c760741e6b7ed43 (MD5)<br>Fundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP)<br>O estudo da formação de planetas terrestres no Sistema Solar, é crucial para compre- endermos como outros sistemas planetários formam e também inferir as condições que poderiam ter influenciado a origem e evolução de vida na Terra. Esta Tese de douto- rado apresenta um e

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Costa, André Izidoro Ferreira da. "Estudos da formação de planetas terrestres /." Guaratinguetá, 2013. http://hdl.handle.net/11449/102493.

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Orientador: Othon Cabo Winter<br>Coorientador: Massayoshi Tsuchida<br>Banca: Tadashi Yokoyama<br>Banca: Nelson Callegari Junior<br>Banca: Roberto Vieira Martins<br>Banca: Fernando Virgilio Roig<br>Resumo: O estudo da formação de planetas terrestres no Sistema Solar, é crucial para compre- endermos como outros sistemas planetários formam e também inferir as condições que poderiam ter influenciado a origem e evolução de vida na Terra. Esta Tese de douto- rado apresenta um estudo numérico da formação de planetas terrestres. Nosso objetivo principal é analisar o último estágio da formação desses p

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Komacek, Thaddeus D., and Andrew N. Youdin. "Structure and Evolution of Internally Heated Hot Jupiters." IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/625158.

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Hot Jupiters receive strong stellar irradiation, producing equilibrium temperatures of 1000-2500 K. Incoming irradiation directly heats just their thin outer layer, down to pressures of similar to 0.1 bars. In standard irradiated evolution models of hot Jupiters, predicted transit radii are too small. Previous studies have shown that deeper heating-at a small fraction of the heating rate from irradiation-can explain observed radii. Here we present a suite of evolution models for HD 209458b, where we systematically vary both the depth and intensity of internal heating, without specifying the un

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Cauley, P. Wilson, Seth Redfield, Adam G. Jensen, and Travis Barman. "VARIATION IN THE PRE-TRANSIT BALMER LINE SIGNAL AROUND THE HOT JUPITER HD 189733B." IOP PUBLISHING LTD, 2016. http://hdl.handle.net/10150/621234.

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As followup to our recent detection of a pre-transit signal around HD 189733 b, we obtained full pre-transit phase coverage of a single planetary transit. The pre-transit signal is again detected in the Balmer lines but with variable strength and timing, suggesting that the bow shock geometry reported in our previous work does not describe the signal from the latest transit. We also demonstrate the use of the Ca II H and K residual core flux as a proxy for the stellar activity level throughout the transit. A moderate trend is found between the pre-transit absorption signal in the 2013 data and

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Biller, Beth A., Johanna Vos, Esther Buenzli, et al. "Simultaneous Multiwavelength Variability Characterization of the Free-floating Planetary-mass Object PSO J318.5−22." IOP PUBLISHING LTD, 2018. http://hdl.handle.net/10150/627034.

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We present simultaneous Hubble Space Telescope (HST) WFC3+Spitzer IRAC variability monitoring for the highly variable young (similar to 20 Myr) planetary-mass object PSO J318.5-22. Our simultaneous HST + Spitzer observations covered approximately two rotation periods with Spitzer and most of a rotation period with the HST. We derive a period of 8.6. +/-. 0.1 hr from the Spitzer light curve. Combining this period with the measuredvsinifor this object, we find an inclination of 56 degrees.2. +/-. 8 degrees.1. We measure peak-to-trough variability amplitudes of 3.4%. +/-. 0.1% for Spitzer Channel

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