Dissertations / Theses on the topic 'Variable stars'
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Davey, Stephen. "Irradiation of the secondary star in cataclysmic variable stars." Thesis, University of Sussex, 1994. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.386388.
Full textKube, Jens. "Indirect imaging of cataclysmic variable stars." Doctoral thesis, [S.l.] : [s.n.], 2002. http://webdoc.sub.gwdg.de/diss/2002/kube/kube.pdf.
Full textThoroughgood, Timothy David. "The masses of cataclysmic variable stars." Thesis, University of Sheffield, 2005. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.419603.
Full textMarsh, T. R. "Emission lines in cataclysmic variable stars." Thesis, University of Cambridge, 1985. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.372891.
Full textSahman, David. "The evolution of cataclysmic variable stars." Thesis, University of Sheffield, 2018. http://etheses.whiterose.ac.uk/21700/.
Full textWynn, Graham Anthony. "Accretion processes in cataclysmic variable stars." Thesis, University of Leicester, 1993. http://hdl.handle.net/2381/35833.
Full textPretorius, Magaretha L. "Rapid oscillations in cataclysmic variable stars." Master's thesis, University of Cape Town, 2004. http://hdl.handle.net/11427/6103.
Full textRapid quasi-coherent oscillations were detected in the optical light curves of 24 cataclysmic variable stars (CVS). In 12 of these systems (TU Men, WW Cet, HX Peg, BP CrA, BR Lup, HP Nor, AG Hya, TW Vir, PU CMa, V426 Ooph, V1193 Ori, and CR Boo) for the first time. The results contribute to the observational record of the phenomenology of dwarf nova oscillations (DNOs), quasi-periodic oscillations (QPOs), and longer period dwarf nova oscillations (lpDNOs), strengthen the correlation, valid over nearly six orders of magnitude in frequency, between the ratio of time scales of different classes of oscillations in white dwarf, neutron star, and black hole binaries, and show that the recently recognized lpDNOs occur fairly commonly in high mass transfer rate CVs.
Ireland, Michael. "Optical interferometry and Mira variable stars /." Connect to full text, 2005. http://hdl.handle.net/2123/721.
Full textIreland, Michael James. "Optical Interferometry and Mira Variable Stars." Thesis, The University of Sydney, 2005. http://hdl.handle.net/2123/721.
Full textIreland, Michael James. "Optical Interferometry and Mira Variable Stars." University of Sydney. Physics, 2005. http://hdl.handle.net/2123/721.
Full textTodd, I. G. "Variable stars as distance indicators in M31." Thesis, Queen's University Belfast, 2008. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.492481.
Full textWynn, Rebecca. "Accretion disc instabilities in cataclysmic variable stars." Thesis, University of Leicester, 2000. http://hdl.handle.net/2381/30642.
Full textHickman, Richard D. G. "Multi-wavelength observations of cataclysmic variable stars." Thesis, University of Warwick, 2011. http://wrap.warwick.ac.uk/38153/.
Full textSmith, Deneal Anthony. "An observational study of cataclysmic variable stars." Thesis, University of Cambridge, 1999. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.624581.
Full textGreenwood, Aaron James. "Spectroscopic Analysis of γ Doradus Variable Stars." Thesis, University of Canterbury. Physics and Astronomy, 2014. http://hdl.handle.net/10092/9216.
Full textFeline, William James. "ULTRACAM photometry of eclipsing cataclysmic variable stars." Thesis, University of Sheffield, 2005. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.425598.
Full textBaskill, Darren Stuart. "X-ray properties of cataclysmic variable stars." Thesis, University of Leicester, 2003. http://hdl.handle.net/2381/30669.
Full textRomero, Daniela. "Comparing the Period-Luminosityrelationships in variable stars." Thesis, Uppsala universitet, Institutionen för fysik och astronomi, 2017. http://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-323634.
Full textHodder, Philip Jeremy Crichton. "A search for faint variable stars in the globular cluster M71." Thesis, University of British Columbia, 1990. http://hdl.handle.net/2429/28830.
Full textScience, Faculty of
Physics and Astronomy, Department of
Graduate
Barker, John. "Driving mechanisms for cataclysmic variable evolution." Thesis, Open University, 2003. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.289006.
Full textPapakonstantinou, Nikolaos. "Investigation of variable Ap Stars in TESS continuous viewing zone." Thesis, Uppsala universitet, Observationell astrofysik, 2021. http://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-441349.
Full textDunlap, Mickey Paul. "Using the bootstrap to analyze variable stars data." Diss., Texas A&M University, 2004. http://hdl.handle.net/1969.1/1398.
Full textWeldrake, David Thomas Fredrick, and weldrake@mpia-hd mpg de. "Giant Planets and Variable Stars in Globular Clusters." The Australian National University. Research School of Astronomy and Astrophysics, 2005. http://thesis.anu.edu.au./public/adt-ANU20050616.191315.
Full textThomas, Nigel Leslie. "Optical and infrared observations of cataclysmic variable stars." Thesis, Open University, 2009. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.497399.
Full textPoole, Tracey Suzanne. "A multi-wavelength study of cataclysmic variable stars." Thesis, University College London (University of London), 2004. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.415225.
Full textNorth, Rachel Caroline. "Probing the system parameters of cataclysmic variable stars." Thesis, University of Southampton, 2001. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.390623.
Full textUnda-Sanzana, Eduardo. "A spectroscopic analysis of three cataclysmic variable stars." Thesis, University of Southampton, 2005. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.414368.
Full textFernley, J. A. "Optical and infrared observations of pulsating variable stars." Thesis, University of Leicester, 1985. http://hdl.handle.net/2381/35882.
Full textBrooks, A. "Short period variable stars in the Kepler field." Thesis, University College London (University of London), 2014. http://discovery.ucl.ac.uk/1447063/.
Full textWeldrake, 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.
Full textHoard, Donald Wayne. "Accretion and structure in the SW Sextantis stars /." Thesis, Connect to this title online; UW restricted, 1998. http://hdl.handle.net/1773/5419.
Full textWoodruff, Henry Christian A. "Optical and infrared aperture masking interferometry of mira variable stars." Thesis, The University of Sydney, 2009. https://hdl.handle.net/2123/28457.
Full textSmits, Derck Peter. "Atomic processes in nova shells." Doctoral thesis, University of Cape Town, 1990. http://hdl.handle.net/11427/16000.
Full textThe unusual spectra of the spatially-resolved nova shells of DQ Her, T Aur and CP Pup are reviewed. Because calculations for these conditions have not been made, recombination models of HI, HeI and CNO from a neutral to a doubly ionized state were constructed. The models are described and the results presented for densities at various temperatures. A photoionization model is also described. The effects of non-uniform density distributions in nova shells have been investigated and the observational consequences discussed. A model of the CP Pup shell is described and the evolution of this plasma during the nova's constant luminosity phase traced. The properties of neon novae are summarized and compared with the features seen in the optical spectra of old classical novae. Enhanced neon abundances are used in the model of the CP Pup Shell to investigate its effect on the evolution of the shell. Finally, the results of some near-infrared observations made on the shells of CP Pup, RR Pic and T Pyx are reported.
Hartley, Louise Elizabeth. "Observation and outflow modelling of luminous cataclysmic variable stars." Thesis, Imperial College London, 2003. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.407959.
Full textPretorius, Magaretha Le Riche. "Observational constraints on the evolution of cataclysmic variable stars." Thesis, University of Southampton, 2008. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.485009.
Full textBass, Gideon. "Ensemble supervised and unsupervised learning with Kepler variable stars." Thesis, George Mason University, 2016. http://pqdtopen.proquest.com/#viewpdf?dispub=10027479.
Full textVariable star analysis and classification is an important task in the understanding of stellar features and processes. While historically classifications have been done manually by highly skilled experts, the recent and rapid expansion in the quantity and quality of data has demanded new techniques, most notably automatic classification through supervised machine learning. I present a study on variable stars in the Kepler field using these techniques, and the novel work of unsupervised learning. I use new methods of characterization and multiple independent classifiers to produce an ensemble classifier that equals or matches existing classification abilities. I also explore the possibilities of unsupervised learning in making novel feature discovery in stars.
Caddy, Robert V. "Time Series Photometry of the Symbiotic Star V1835 Aql and New Variable Stars in Aquila." Bowling Green State University / OhioLINK, 2018. http://rave.ohiolink.edu/etdc/view?acc_num=bgsu1525438143057776.
Full textPENNING, WILLIAM ROY. "INVESTIGATIONS OF LONG-PERIOD DQ HERCULIS STARS." Diss., The University of Arizona, 1986. http://hdl.handle.net/10150/188161.
Full textCall, Scott. "Long-Period Variable Stars in the Globular Cluster NGC 6553." Bowling Green State University / OhioLINK, 2021. http://rave.ohiolink.edu/etdc/view?acc_num=bgsu1626973295690519.
Full textDrake, A. J., S. G. Djorgovski, M. Catelan, M. J. Graham, A. A. Mahabal, S. Larson, E. Christensen, et al. "The Catalina Surveys Southern periodic variable star catalogue." OXFORD UNIV PRESS, 2017. http://hdl.handle.net/10150/625504.
Full textWoollands, Robyn. "Photometric Analysis of R Coronae Borealis stars in the Magellanic Clouds." Thesis, University of Canterbury. Physics and Astronomy, 2008. http://hdl.handle.net/10092/1876.
Full textDeschamps, Romain. "Evolution of low and intermediate mass stars in binary systems: a new look at Algol systems." Doctoral thesis, Universite Libre de Bruxelles, 2015. http://hdl.handle.net/2013/ULB-DIPOT:oai:dipot.ulb.ac.be:2013/209077.
Full textstill rather poorly understood. We know that they are composed by a generally B-A main sequence
star and a lighter but more evolved companion star. This paradox is explained by the transfer of mass
between the two stars, but new problems arose. In particular, I studied the mass-transfer driven spin-
up of the accreting star that drives the star to critical rotation and the puzzling, indirectly observed, non-conservative evolution.
Doctorat en Sciences
info:eu-repo/semantics/nonPublished
Blakelock, Carolyn J. "Time-resolved spectroscopy of the AM Herculis-type binary systems QQ VUL and EF ERI." Virtual Press, 1998. http://liblink.bsu.edu/uhtbin/catkey/1115429.
Full textDepartment of Physics and Astronomy
Kawka, Adela. "A study of white dwarfs in the solar neighbourhood." Thesis, Kawka, Adela (2003) A study of white dwarfs in the solar neighbourhood. PhD thesis, Murdoch University, 2003. https://researchrepository.murdoch.edu.au/id/eprint/120/.
Full textKawka, Adela. "A study of white dwarfs in the solar neighbourhood." Kawka, Adela (2003) A study of white dwarfs in the solar neighbourhood. PhD thesis, Murdoch University, 2003. http://researchrepository.murdoch.edu.au/120/.
Full textPala, A. F., B. T. Gänsicke, D. Townsley, D. Boyd, M. J. Cook, Martino D. De, P. Godon, et al. "Effective temperatures of cataclysmic-variable white dwarfs as a probe of their evolution." OXFORD UNIV PRESS, 2017. http://hdl.handle.net/10150/623936.
Full textFriedman, Vanessa Ann. "Identifying Long Period Variable (LPV) Stars Using Images from the Stardial Observatory." Thesis, The University of Arizona, 2009. http://hdl.handle.net/10150/193423.
Full textVilardell, Sallés Francesc. "Determination of the distance to the Andromeda Galaxy using variable stars." Doctoral thesis, Universitat de Barcelona, 2009. http://hdl.handle.net/10803/751.
Full textWe obtained high quality light curves (rms~0.01 mag) from a 34'x34' photometric survey in M31 (in Johnson B and V filters) carried out at the 2.5 m Isaac Newton Telescope (La Palma, Spain). This survey provided light curves for almost 4000 variable stars, with over 400 EBs and 400 Cepheids. The 24 brightest EBs (V<20.5 mag) with deeper eclipses (dV>0.2 mag) were selected as optimum candidates for distance determination. Five of these EBs (located in a 5'x5' region) were selected to be observed with the multi-object spectrograph (GMOS) at the Gemini-North telescope. We obtained accurate radial velocities for the four brightest EBs observed with GMOS, enabling the first direct determination of masses and radii of stars in M31. Two of these EBs were used to derive a direct distance determination to M31 of (m-M)o=24.36+/-0.08 mag.
Another system is the most massive EB with apsidal motion ever reported, enabling the analysis of the distribution of matter in the interior of stars with masses larger than 40 Msun. In all cases, the direct determination of masses and radii allowed a direct comparison with stellar evolutionary models, providing the evolutionary stage for each system. In addition to the EB analysis, we also performed a comprehensive study of Cepheids in M31. The obtained results showed that blending is as important as metallicity correction when determining Cepheid distances to Local Group galaxies and provided an additional distance determination to M31 of (m-M)o=24.32+-0.12 mag, fully compatible with the EB distance. Finally, we also discovered a large flare during the acquisition of the photometric catalog. The performed study revealed that the underlying source was a dM star having one of the most energetic flares ever observed.
La Galàxia d'Andròmeda (M31) és un excel·lent calibrador de l'escala cosmològica de distàncies. Presentem la primera determinació directa de la distància a M31 mitjançant binàries eclipsants (EBs). Les EBs proporcionen determinacions directes de la distància perquè les propietats físiques dels seus components es poden mesurar sense cap calibratge previ. Les determinacions de distància a partir de EBs requereixen, almenys, dos tipus d'observacions: series fotomètriques i espectroscòpia. Vam obtenir corbes de llum de gran qualitat (rms~0.01 mag) amb el telescopi Isaac Newton (a La Palma) d'un camp de 34'x34' a M31 (amb els filtres Johnson B i V). Aquest estudi va proporcionar corbes de llum de gairebé 4000 estrelles variables, amb més de 400 EBs i 400 Cefeides.
Les 24 EBs més brillants (V<20.5 mag) i amb eclipsis més profunds (dV>0.2 mag) es van seleccionar com a candidates idònies per determinar-ne la distància. Cinc d'aquestes EBs (situades en una regió de 5'x5') es van selecccionar per observar-se amb l'espectrògraf multiobjecte (GMOS) al telescopi Gemini-North. Vam obtenir velocitats radials d'alta qualitat per a les quatre EBs més brillants observades amb GMOS, permetent la primera determinació directa de masses i radis d'estrelles a M31. Dues d'aquestes EBs van ser utilitzades per obtenir una determinació directa de la distància a M31 de (m-M)o=24.36+/-0.08 mag. Un altre sistema va resultar ser el sistema més massiu amb moviment apsidal mai detectat, permetent l'anàlisi de la distribución de matèria a l'interior de les estrelles amb masses superiors a 40 masses solars. En tots els casos, la determinació directa de les masses i els radis va permetre una comparació directa amb models estel·lars, proporcionant l'estadi evolutiu de cada sistema.
Paral·lelament a l'anàlisi de binàries, vam realitzar un exhaustiu estudi de les Cefeides de M31. Els resultats obtinguts van demostrar que l'efecte de la confusió de diverses fonts (blending) és tant important com la correcció de metal·licitat per a la determinació de distàncies amb Cefeides al Grup Local i van proporcionar una distància addicional a M31 de (m-M)o=24.32+/-0.12 mag, completament compatible amb la distància de les EBs. Finalment, vam descobrir una gran fulguració estel·lar durant l'adquisició del catàleg fotomètric. L'estudi realitzat va revelar que la font era una estrella dM, amb una de les fulguracions més energètiques mai observades.
La Galaxia de Andrómeda (M31) es un excelente calibrador de la escala cosmológica de distancias. Presentamos la primera determinación directa de la distancia a M31 mediante binarias eclipsantes (EBs). Las EBs proporcionan determinaciones directas de la distancia porque las propiedades físicas de sus componentes se pueden medir sin ningún tipo de calibración previa. Las determinaciones de distancia a partir de EBs requieren, como mínimo, dos tipos de observaciones: series fotométricas y espectroscopia. Obtuvimos curvas de luz de gran calidad (rms~0.01 mag) con el telescopio Isaac Newton (en La Palma) en un campo de 34'x34' en M31 (con los filtros Johnson B y V). Este estudio proporcionó curvas de luz para casi 4000 estrellas variables, con más de 400 EBs y 400 Cefeidas. Las 24 EBs más brillantes (V<20.5 mag) y con eclipses más profundos (dV>0.2 mag) se seleccionaron como candidatos idóneos para determinar la distancia. Cinco de estas EBs (situadas en una región de 5'x5') se seleccionaron para ser observadas con el espectrógrafo multiobjeto (GMOS) en el telescopio Gemini-North. Obtuvimos velocidades radiales de alta calidad para las cuatro EBs más brillantes observadas con GMOS, permitiendo la primera determinación directa de masas y radios para estrellas de M31. Dos de estas EBs fueron utilizadas para obtener una determinación directa de la distancia a M31 de (m-M)o=24.36+/-0.08 mag.
Otro sistema resultó ser el sistema más masivo con movimiento apsidal nunca detectado, permitiendo el análisis de la distribución de materia en el interior de las estrellas con masas superiores a 40 masas solares. En todos los casos, la determinación directa de masas y radios permitió una comparación directa con modelos estelares, proporcionando así el estadio evolutivo de cada sistema. Paralelamente al análisis de binarias, realizamos un exhaustivo estudio de las Cefeidas en M31. Los resultados obtenidos demostraron que el efecto de la confusión de varias fuentes (blending) es tan importante como la corrección de metalicidad para la determinación de distancias con Cefeidas en el Grupo Local y proporcionaron una distancia adicional a M31 de (m-M)o=24.32+/-0.12 mag, completamente compatible con la distancia de las EBs. Finalmente, se descubrió una gran fulguración estelar durante la adquisición del catálogo fotométrico. El estudio realizado reveló que la fuente era una estrella dM, presentando una de las fulguraciones más energéticas nunca observadas.
Smitka, Michael Thomas. "Analysis of the Halo Globular Cluster M30 and its Variable Stars." Bowling Green State University / OhioLINK, 2007. http://rave.ohiolink.edu/etdc/view?acc_num=bgsu1182382804.
Full textPellegrin, Kyle S. "Long Period Variable Stars in the Globular Cluster M5 (NGC 5904)." Bowling Green State University / OhioLINK, 2020. http://rave.ohiolink.edu/etdc/view?acc_num=bgsu1595605798891894.
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