Rozprawy doktorskie na temat „Extrasolar planets”
Utwórz poprawne odniesienie w stylach APA, MLA, Chicago, Harvard i wielu innych
Sprawdź 50 najlepszych rozpraw doktorskich naukowych na temat „Extrasolar planets”.
Przycisk „Dodaj do bibliografii” jest dostępny obok każdej pracy w bibliografii. Użyj go – a my automatycznie utworzymy odniesienie bibliograficzne do wybranej pracy w stylu cytowania, którego potrzebujesz: APA, MLA, Harvard, Chicago, Vancouver itp.
Możesz również pobrać pełny tekst publikacji naukowej w formacie „.pdf” i przeczytać adnotację do pracy online, jeśli odpowiednie parametry są dostępne w metadanych.
Przeglądaj rozprawy doktorskie z różnych dziedzin i twórz odpowiednie bibliografie.
Carter, Andrew James. "Observation and modeling of extrasolar planets". Thesis, Open University, 2011. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.578669.
Pełny tekst źródłaMuterspaugh, Matthew Ward. "Binary star systems and extrasolar planets". Thesis, Massachusetts Institute of Technology, 2005. http://hdl.handle.net/1721.1/34646.
Pełny tekst źródłaIncludes bibliographical references (p. 121-137).
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 this, binary stars have often been avoided by programs searching for planets. Discovery of giant planets in compact binary systems would indirectly probe the timescales of planet formation, an important quantity in determining by which processes planets form. A new observing method has been developed to perform very high precision differntial astrometry on bright binary stars with separations in the range of 0.1 - 1.0 arcseconds. Typical measurement precisions over an hour of integration are on the order of 10 micro-arcseconds (as), enabling one to look for perturbations to the Keplerian orbit that would indicate the presence of additional components to the system. This method is used as the basis for a new program to find extrasolar planets. The Palomar High-precision Astrometric Search for Exoplanet Systems (PHASES) is a search for giant planets orbiting either star in 50 binary systems. The goal of this search is to detect or rule out planets in the systems observed and thus place limits on any enhancements of planet formation in binaries. It is also used to measure fundamental properties of the stars comprising the binary, such as masses and distances, useful for constraining stellar models at the 10-3 level.
(cont.) This method of differential astrometry is applied to three star systems. Equulei is among the most well-studied nearby binary star systems. Results of its observation have been applied to a wide range of fundamental studies of binary systems and stellar astrophysics. PHASES data are combined with previously published radial velocity data and other previously published differential astrometry measurements to produce a combined model for the system orbit. The distance to the system is determined to within a twentieth of a parsec and the component masses are determined at the level of a percent. n Pegasi is a well-known, nearby triple star system consisting of a "wide" pair with semi-major axis 235 milli-arcseconds, one component of which is a single-line spectroscopic binary (semi-major axis 2.5 milli-arcseconds). Using high-precision differential astrometry and radial velocity observations, the masses for all three components are determined and the relative inclination between the wide and narrow pairs' orbits is found to be 43.8 ± 3.0 degrees, just over the threshold for the three body Kozai resonance. The system distance is determined to a fifth of a parsec, and is consistent with trigonometric parallax measurements. V819 Herculis is a well-studied triple star system consisting of a "wide" pair with 5.5 year period, one component of which is a 2.2-day period eclipsing single-line spectroscopic binary. Differential astrometry measurements from PHASES determine the relative inclination of the short- and long-period orbits. Finally, the prospects for finding planets that simultaneously circle both stars in a binary system are evaluated. Planet searches of this type would represent a complementary investigation to PHASES and contribute similar scientific results.
by Matthew Ward Muterspaugh.
Ph.D.
Hood, Ben Andrew Ashcom. "Extrasolar planet search and characterisation". Thesis, St Andrews, 2007. http://hdl.handle.net/10023/359.
Pełny tekst źródłaDominis, Dijana. "The role of binary stars in searches for extrasolar planets by microlensing and astrometry". Phd thesis, Universität Potsdam, 2006. http://opus.kobv.de/ubp/volltexte/2006/1081/.
Pełny tekst źródłaLeigh, Christopher. "The detection and characterisation of extrasolar planets". Thesis, University of St Andrews, 2004. http://hdl.handle.net/10023/12943.
Pełny tekst źródłaDoellinger, Michaela. "Hunting for extrasolar planets around K giants". Diss., lmu, 2008. http://nbn-resolving.de/urn:nbn:de:bvb:19-99700.
Pełny tekst źródłaNikku, Madhusudhan 1980. "Retrieval of atmospheric properties of extrasolar planets". Thesis, Massachusetts Institute of Technology, 2009. http://hdl.handle.net/1721.1/63006.
Pełny tekst źródłaCataloged from PDF version of thesis.
Includes bibliographical references (p. 133-137).
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, hydrostatic equilibrium, and energy balance, along with prescriptions for non-equilibrium molecular composition and energy redistribution. The major difference from traditional 1-D radiative transfer models is the parametric P-T profile, which essentially means adopting energy balance only at the top of the atmosphere and not in each layer. We see the parametric P-T model as a parallel approach to the traditional exoplanet atmosphere models that rely on several free parameters to encompass unknown absorbers and energy redistribution. The parametric P-T profile captures the basic physical features of temperature structures in planetary atmospheres (including temperature inversions), and reproduces a wide range of published P-T profiles, including those of solar system planets. We apply our temperature and abundance retrieval method to two exoplanets which have the best data available, HD 189733b and HD 209458b. For each planet, we compute - 107 atmospheric spectra on a grid in the parameter space, and report contours of the error surface, given the data. For the day-side of HD 189733b, we place constraints on the atmospheric properties based on three different data sets available. Our best-fit models to one of the data sets allow for very efficient daynight energy redistribution in HD 189733b. The different constraints on molecular abundances confirm the presence of H20, CH4 , CO and CO 2 in HD 189733b. Our results also rule out the presence of a thermal inversion in this planet. The model constraints due to the different data sets indicate that the planetary atmosphere is variable, both, in its energy redistribution state and in the chemical abundances. The variability is evident in the data; some key observations with different instruments at the same wavelength differ at the - 2- level. If, on the other hand, the differences in data represent underestimated errors, and if all the data sets have to be reconciled simultaneously, then we are unable to make specific constraints on the molecular abundances or on the temperature profile, beyond identification of molecules and the presence or absence of a thermal inversion. For HD 209458b, we confirm and constrain a thermal inversion in the day-side atmosphere, and the data allows for very efficient day-night redistribution of energy. We report detection of CO, CH4 and CO 2 on the dayside of HD 209458b, along with placing an upper-limit on the amount of H2 0. We also report atmospheric models for three transiting exoplanets with limited data: TrES-2, HAT-P-7b, GJ 436b. For TrES-2 and HAT-P-7b, where only four observations each are available, we find that the data can be fit with models with and without thermal inversions, if we make no assumptions of chemical equilibrium. Finally, in this work, we report the first steps towards developing a parameter estimation procedure for exoplanetary atmospheres. We demonstrate with simulated data that our model can be used with a formal Bayesian parameter estimation algorithm, like MCMC, to place constraints on the atmospheric properties of hot Jupiters.
by Nikku, Madhusudhan.
Ph.D.
Kipping, D. M. "The transits of extrasolar planets with moons". Thesis, University College London (University of London), 2011. http://discovery.ucl.ac.uk/1306758/.
Pełny tekst źródłaGaudi, B. Scott. "Microlensing and the search for extrasolar planets /". The Ohio State University, 2000. http://rave.ohiolink.edu/etdc/view?acc_num=osu1488199501405399.
Pełny tekst źródłaLewis, Nikole Kae. "Atmospheric Circulation of Eccentric Extrasolar Giant Planets". Diss., The University of Arizona, 2012. http://hdl.handle.net/10150/242352.
Pełny tekst źródłaSissa, Elena. "Observation of extrasolar planets at various ages". Doctoral thesis, Università degli studi di Padova, 2017. http://hdl.handle.net/11577/3426311.
Pełny tekst źródłaLa ricerca e la caratterizzazione dei pianeti extrasolari è uno dei maggiori campi di ricerca dell’astronomia attuale, con lo scopo ultimo di capire i meccanismi di formazione e di evoluzione dei sistemi planetari, le condizioni che permettono la formazione di ambienti adatti alla vita, e di trovare le prove di vita extra-solare. Negli ultimi decenni, la ricerca dei pianeti extrasolari ha visto un rapido aumento di interesse, e sono state cosí sviluppate nuove metodologie di ricerca. Ognuna di esse ha aspetti positivi e negativi per lo studio dell’architettura dei sistemi extrasolari e la caratterizzazione dei pianeti. Le stelle e il loro entourage planetario si formano e crescono assieme, per lo meno nella maggioranza dei casi, legate dal disco circumstellare. Al momento manca una teoria universale che possa descrivere tutti i processi che accadono tra le fasi del collasso della nube protostellare e la stabilizzazione finale del sistema. I metodi indiretti sono molto utili per studiare le zone interne dei sistemi più evoluti, nei quali il contributo del disco protoplanetario è trascurabile. Dall’altro lato, la tecnica dell’imaging diretto con strumenti ad alto contrasto offre la possibilità di studiare le prime fasi della formazione planetaria, non accessibili con altri metodi indiretti, e gioca un ruolo fondamentale per le attuali teorie di formazione planetaria. Questa tesi si focalizza sulle capacità dell’imaging diretto ottenuto con SPHERE, il nuovo strumento ad alto contrasto del VLT, nel rivelare pianeti in diversi stadi della loro evoluzione, e presenta uno studio complementare di sistemi vecchi basato sulle osservazioni delle velocità radiali con SARG, il vecchio spettrografo echelle del TNG. Il Capitolo 1 introduce brevemente le teorie di formazione ed evoluzione dei pianeti con i più importanti metodi di ricerca. Il Capitolo \ref{sec:sphere} descrive SPHERE, lo strumento usato per la maggior parte dei risultati presentati in questa tesi. Nel Capitolo 3 presento il caso di quattro oggetti giovani. Ho sfruttato il canale visibile di SPHERE per studiare i jet di Z CMa, e il canale nel vicino infrarosso per HD 100546 e T Cha, cercando segnali della presenza di pianeti. Allo stesso tempo, ho potuto studiare in dettaglio il disco circumstellare di HD 100546 in un intervallo spettrale relativamente ampio: nella sezione ad esso dedicata mostra che le strutture più brillanti del sistema suggeriscono la presenza di almeno tre regioni vuote nelle zone interne del disco, assieme ad altre strutture, come ad esempio bracci a spirale. Ho anche rilevato la presenza di una sorgente diffusa nella posizione attesa per il potenziale pianeta b, ma la natura di questa emissione è, tuttavia, ancora sconosciuta. Infine, LkCa 15 è stato studiato sia nel canale visibile che in quello del vicino infrarosso di SPHERE. Nel Capitolo 4 presento lo studio dei segni distintivi di accrescimento in un gruppo di oggetti. L’accrescimento di GQ Lup b è stato osservato sia in H_alpha che il Paschen beta, sfruttando tutti e tre i sottosistemi di SPHERE. Due sistemi i cui dintorni sono già stati ripuliti dal gas e dalla polvere sono presentati nel Capitolo 5: HIP 80591 e HIP 65426. In quest’ultimo, ho scoperto che uno dei candidati compagni aveva un’alta probabilità di essere legato alla stella a causa della sua posizione e delle sue caratteristiche spettrali. Queste conclusioni sono state poi confermate da un’analisi approfondita e da ulteriori osservazioni che hanno dimostrato che quel compagno, HD 65426 b, è un pianeta gioviano caldo con massa compresa tra 6 e 12 M_J. Nel Capitolo 6, studio l’attività cromosferica in stelle binarie vecchie allo scopo di identificare un segnale nelle velocità radiali nascosto dallo spostamento Doppler indotto dall’attività. Ho scoperto che Ha-excess, un indice basato sulla riga \Ha, è un buon indicatore dell’attività stellare quando l’indice \RHK\ non è disponibile e può essere anche usato per derivare l’età delle stelle nel caso siano più giovani di 1.5 Gyr. Inoltre, HD 76037 B mostra una variazione elevata delle velocità radiali che puo’ essere spiegata con la presenza di un compagno di piccola massa (Sissa et al. 2017) Infine, nel Capitolo 7 fornisco le conclusioni del lavoro ed espongo sviluppi futuri. Le appendici sono dedicate agli aspetti più tecnici del mio lavoro, che sono stati necessari per migliorare le capacità dello strumento e la riduzione dei dati, e per definire al meglio i set-up necessari allo strumento per raggiungere i differenti scopi scientifici.
Steffen, Jason. "Detecting new planets in transiting systems /". Thesis, Connect to this title online; UW restricted, 2006. http://hdl.handle.net/1773/9686.
Pełny tekst źródłaVeras, Dimitri George. "The orbital evolution of extrasolar planets after formation". Connect to online resource, 2007. http://gateway.proquest.com/openurl?url_ver=Z39.88-2004&rft_val_fmt=info:ofi/fmt:kev:mtx:dissertation&res_dat=xri:pqdiss&rft_dat=xri:pqdiss:3273687.
Pełny tekst źródłaWilson, David M. "The search for transiting extrasolar planets with SuperWASP". Thesis, Keele University, 2007. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.443609.
Pełny tekst źródłaKoskinen, T. T. "The stability of short-period extrasolar giant planets". Thesis, University College London (University of London), 2008. http://discovery.ucl.ac.uk/1444248/.
Pełny tekst źródłaMengistie, Getachew Mekonnen. "Gravitational microlensing and the search for extrasolar planets". Master's thesis, University of Cape Town, 2013. http://hdl.handle.net/11427/9798.
Pełny tekst źródłaThis project is aimed at tackling binary gravitational microlensing events. Since the early conception of gravitational lensing before Einstein’s General Theory of Relativity, physicists and astronomers of the early 18th century speculated that light, if treated as particle, can be affected by gravitational field. Gravitational Microlensing is defined as a phenomenon occurring when light coming from a distant (source) star is bent by the gravitational field of an intervening mass (lens) creating multiple image of the source which cannot be resolved. In this project, We applied a model for binary lens microlensing events. We analysed data obtained from different observatories: PLAXET, which includes SAAO, Sutherland, Canopus and Perth observatories, OGLE, Danish Telescope, LaSilla. For the observed microlensing target OGLE-2011-BLG-265, analysis of the data using the program supplied by Keith Horne, using different minimization schemes and algorithms, I found best fit model to be a binary lens with mass ratio q = 0.0042 and separation of components is found to be u = 1.034 where in this case the separation falls under an intermediate binary lens topology. Finally, the deviation from the point-source point-lens microlensing events on the light curve and small mass ratio suggested a planetary system. I also calculated the time, tp, that the source needs to cross the diameter of the planet Einstein Ring radius, which is related to the mass ratio, and is found to be 3.30 days.
Safizadeh, Neda. "Detection of extrasolar planets via microlensing and occultation /". Diss., Connect to a 24 p. preview or request complete full text in PDF format. Access restricted to UC campuses, 2001. http://wwwlib.umi.com/cr/ucsd/fullcit?p3001275.
Pełny tekst źródłaCooper, Curtis Steven. "Meteorologies of Brown Dwarfs and Extrasolar Giant Planets". Diss., The University of Arizona, 2006. http://hdl.handle.net/10150/195544.
Pełny tekst źródłaSudarsky, David. "Theoretical spectra and atmospheres of extrasolar giant planets". Diss., The University of Arizona, 2002. http://hdl.handle.net/10150/280087.
Pełny tekst źródłaTan, Xianyu, i 谭先瑜. "Characterizing the orbital and dynamical state of extrasolar multiple-planet systems with radial velocity measurements". Thesis, The University of Hong Kong (Pokfulam, Hong Kong), 2013. http://hub.hku.hk/bib/B50162792.
Pełny tekst źródłapublished_or_final_version
Earth Sciences
Master
Master of Philosophy
Lavvas, P., i T. Koskinen. "Aerosol Properties of the Atmospheres of Extrasolar Giant Planets". IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/626046.
Pełny tekst źródłaCiceri, Simona [Verfasser], i Thomas [Akademischer Betreuer] Henning. "Characterizing Transiting Extrasolar Planets / Simona Ciceri ; Betreuer: Thomas Henning". Heidelberg : Universitätsbibliothek Heidelberg, 2016. http://d-nb.info/1180610245/34.
Pełny tekst źródłaThrastarson, Heidar Thor. "General circulation modelling of close-in extrasolar giant planets". Thesis, Queen Mary, University of London, 2011. http://qmro.qmul.ac.uk/xmlui/handle/123456789/2448.
Pełny tekst źródłaBurton, John Robert. "Ground-based investigations of the atmospheres of extrasolar planets". Thesis, Queen's University Belfast, 2014. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.669663.
Pełny tekst źródłaBerton, Alessandro. "Detecting extrasolar planets using IFS-based simultaneous differential imaging". [S.l. : s.n.], 2006. http://nbn-resolving.de/urn:nbn:de:bsz:16-opus-70936.
Pełny tekst źródłaBarton, Emma Jane. "Hot molecular line lists for extrasolar planets and industry". Thesis, University College London (University of London), 2016. http://discovery.ucl.ac.uk/1508500/.
Pełny tekst źródłaChristiaens, Valentín André. "Imaging of interactions between circumstellar disks and extrasolar planets". Tesis, Universidad de Chile, 2018. http://repositorio.uchile.cl/handle/2250/168078.
Pełny tekst źródłaSe necesitan observaciones para restringir los mecanismos involucrados en el proceso de formación de planetas. Los discos circunestelares ricos en gas y polvo, llamados discos protoplanetarios, son el lugar esperado de nacimiento de los planetas. Esta tesis se aprovecha de la sinergia entre ALMA y los instrumentos de imagen de alto contraste (HCI) para estudiar la formación de planetas y la retroalimentación mutua planeta-disco en discos protoplanetarios con grandes huecos, llamados discos de transición. La primera parte de esta tesis está dedicada a la imagen de estos discos. En particular, se realizó un análisis detallado de las espirales encontradas en MWC 758 y HD 142527. Las espirales de MWC 758 son probablemente debidas a la presencia de dos compañeros, con uno de ellos posiblemente detectado dentro de la cavidad en base a nuestros datos. En el caso de HD 142527, las espirales del borde de la cavidad parecen ser, junto con otras características del disco, productos de la interacción dinámica entre la binaria y el disco. Las espirales frías a mayor escala vistas con ALMA podrían estar relacionadas con la inestabilidad gravitacional del disco o las sombras proyectadas por el disco interno inclinado. Para probar la hipótesis que los huecos grandes en los discos de transición se deben a la presencia de compañeros, se llevó a cabo una encuesta HCI de esos discos utilizando VLT/NACO en IR térmico, presentada en la segunda parte de esta tesis. Se implementaron códigos de reducción de datos que se utilizaron para buscar compañeros en todos los discos ya observados en esta encuesta. Hasta el momento, se han identificado cuatro candidatos compañeros (de 15 fuentes observadas), aunque se requiere seguimiento para confirmar que son verdaderos compañeros. También se presenta mi contribución a la detección de un compañero subestelar joven muy rojo en el disco de escombros de HD 206893. El potencial de los espectrógrafos de campo integral (IFS) para detectar y caracterizar compañeros de baja masa está investigado en la tercera parte de esta tesis. Se observó una muestra de cinco discos de transición usando VLT/SINFONI en infrarojo cercano. La combinación de imagen diferencial angular y espectral (ASDI) permitió suprimir las imperfecciones del halo estelar de manera eficaz y lograr altos contrastes. Se detectaron tres compañeros y dos sistemas con espirales. En particular, se detectó el compañero de baja masa HD 142527 B en la mayoría de los canales espectrales lo que permitió llevar a cabo una caracterización espectral detallada y estimar sus parámetros físicos. En conclusión, esta tesis provee nueva información sobre los discos de transición y el posible vínculo entre los grandes huecos y la presencia de compañeros. Un análisis similar al caso de HD 142527 se aplicará a los compañeros confirmados en nuestras encuestas para entender mejor las interacciones compañero-disco y la formación de planetas.
Este trabajo ha sido parcialmente financiado por CONICYT-PCHA/Doctorado Nacional/2016-21161112
Bond, Jade. "The Chemistry of Extrasolar Planetary Systems". Diss., The University of Arizona, 2008. http://hdl.handle.net/10150/194946.
Pełny tekst źródłaMustill, Alexander James. "The dynamics of planets and discs". Thesis, University of Cambridge, 2012. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.610345.
Pełny tekst źródłaChristiansen, Jessie Leigh Physics Faculty of Science UNSW. "A tale of two surveys: searching for extrasolar planets from Australia and Antarctica". Awarded By:University of New South Wales. Physics, 2007. http://handle.unsw.edu.au/1959.4/43629.
Pełny tekst źródłaBaines, Ellyn. "Inspection and characterization of exoplanet systems using the CHARA Array". unrestricted, 2007. http://etd.gsu.edu/theses/available/etd-08062007-165009/.
Pełny tekst źródłaTitle from file title page. Harold A. McAlister, committee chair; Todd J. Henry, Douglas R. Gies, Theo A. ten Brummelaar, Nikolaus Dietz, committee members. Electronic text ( 433 p. : ill.) : digital, PDF file. Description based on contents viewed Oct. 29, 2007. Includes bibliographical references (p. 184-194).
Chan, Ka-ho, i 陳嘉豪. "Numerical exploration of the probability of capture into the 3:1 mean motion resonance". Thesis, The University of Hong Kong (Pokfulam, Hong Kong), 2013. http://hub.hku.hk/bib/B4979971X.
Pełny tekst źródłapublished_or_final_version
Physics
Master
Master of Philosophy
Hamacher, Duane Willis Physics Faculty of Science UNSW. "A search for transiting extrasolar planets from the southern hemisphere". Publisher:University of New South Wales. Physics, 2008. http://handle.unsw.edu.au/1959.4/40943.
Pełny tekst źródłaFjällmyr, Lennart. "En bibliometrisk kartläggning av det astronomiska/astrofysikaliska forskningsområdet ”extrasolar planets”". Thesis, Högskolan i Borås, Institutionen Biblioteks- och informationsvetenskap / Bibliotekshögskolan, 2010. http://urn.kb.se/resolve?urn=urn:nbn:se:hb:diva-19862.
Pełny tekst źródłaGallardo, José. "Physics of low mass stars, brown dwarfs and extrasolar planets". Lyon, École normale supérieure (sciences), 2007. http://www.theses.fr/2007ENSL0412.
Pełny tekst źródłaAlsubai, Khalid. "Wide angle search for extrasolar planets by the transit method". Thesis, St Andrews, 2008. http://hdl.handle.net/10023/521.
Pełny tekst źródłaDittmann, Jason A. "Observing Extrasolar Planets at the University of Arizona's Kuiper Telescope". Thesis, The University of Arizona, 2010. http://hdl.handle.net/10150/146800.
Pełny tekst źródłaMorgan, Rhonda Michelle. "Achromatic nulling beam combiner for the detection of extrasolar planets". Diss., The University of Arizona, 2001. http://hdl.handle.net/10150/279844.
Pełny tekst źródłaWeldrake, David Thomas Frederick. "Giant planets and variable stars in globular clusters /". View thesis entry in Australian Digital Theses Program, 2005. http://thesis.anu.edu.au/public/adt-ANU20050616.191315/index.html.
Pełny tekst źródłaGrether, Daniel Andrew Physics Faculty of Science UNSW. "Statistical analyses of extrasolar planets and other close companions to nearby stars". Awarded by:University of New South Wales. School of Physics, 2006. http://handle.unsw.edu.au/1959.4/29182.
Pełny tekst źródłaVoss, Holger. "Developing a ground-based search system for transits of extrasolar planets". [S.l.] : [s.n.], 2006. http://opus.kobv.de/tuberlin/volltexte/2006/1354/index.html.
Pełny tekst źródłaHidas, M??rton Gergely Physics Faculty of Science UNSW. "A search for transiting extrasolar planets with the automated patrol telescope". Awarded by:University of New South Wales. School of Physics, 2005. http://handle.unsw.edu.au/1959.4/22803.
Pełny tekst źródłaKains, Noé. "The Solar System in perspective : from debris discs to extrasolar planets". Thesis, University of St Andrews, 2010. http://hdl.handle.net/10023/1030.
Pełny tekst źródłaAnderson, David Robert. "The discovery and characterisation of the extrasolar planets of WASP-South". Thesis, Keele University, 2013. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.602973.
Pełny tekst źródłaBarnes, Jason Wayne. "Characterizing transiting extrasolar giant planets: On companions, rings, and love handles". Diss., The University of Arizona, 2004. http://hdl.handle.net/10150/290019.
Pełny tekst źródłaGranata, Valentina. "Numerical algorithms for the searching of extrasolar planets from photometric data". Doctoral thesis, Università degli studi di Padova, 2008. http://hdl.handle.net/11577/3425016.
Pełny tekst źródłaStreet, Rachel. "A search for extra-solar planetary transits in the field of open cluster NGC 6819". Thesis, University of St Andrews, 2002. http://hdl.handle.net/10023/12939.
Pełny tekst źródłaBiller, Beth Alison. "A High Contrast Survey for Extrasolar Giant Planets with the Simultaneous Differential Imager (SDI)". Diss., The University of Arizona, 2007. http://hdl.handle.net/10150/194542.
Pełny tekst źródłaBarker, Adrian John. "Tidal interactions between planets and stars". Thesis, University of Cambridge, 2011. https://www.repository.cam.ac.uk/handle/1810/240581.
Pełny tekst źródłaGriessmeier, Jean-Mathias. "Aspects of the magnetosphere-stellar wind interaction of close-in extrasolar planets". Phd thesis, Katlenburg-Lindau Copernicus GmbH, 2006. http://www.digibib.tu-bs.de/?docid=00013336.
Pełny tekst źródła