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Investigation of outburst characteristics in dwarf novae binary star systemsKlep, James Stuart. January 2009 (has links)
Dwarf novae are a type of binary star system that consists of a cool red dwarf, as well as a white dwarf with an accretion disk. Occasionally the disk will get significantly brighter for a few days in an event called an outburst. On February 6th, 2002 one such system, CN Orionis, was experiencing such an outburst. The goal of this research was to determine some important characteristics of CN Orionis during its outburst. This thesis will present the light output, temperature, and the area of the accretion disk of CN Orionis. / Department of Physics and Astronomy
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Spectroscopic analysis of the dwarf nova SS CygniBenson-Avillan, Elixia. January 2010 (has links)
Dwarf novae are a type of cataclysmic variable in which one of the components is
a white dwarf. Their outbursts can range in brightness from two to five magnitudes at
intervals that can vary from days to decades. The purpose of this study is to analyze the
outburst of SS Cygni on the nights of June 18-22, 1987. Using an Interactive Reduction
Software (IRS) package and a Gaussian fit program, the emission and absorption line
strengths on the rise to outburst showed an increase in the flux as well as various other
details supported by theory. / Dwarf novae -- Accretion disk -- SS Cygni -- Data analysis and results. / Department of Physics and Astronomy
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Accretion disk radii changes in IP Peg during outburstHamper, Randall T. January 2007 (has links)
The focus of this study is the change in accretion disk size in Dwarf Novae (DN), IP Peg. DN systems are a type of cataclysmic variable that experience periodic outbursts. These outbursts are caused by the release of gravitational potential energy from an increased rate of matter flow through the accretion disk. Throughout outburst, the radius of the accretion disk of the DN changes. Recent research done at Ball State University has suggested that the disk radius may not change as the disk instability model predicts. According to the disk instability model, the accretion disk should be at its largest radial size when the DN is at the peak of outburst. IP Peg in September and October of 2006 underwent outburst. It was found that during that particular outburst that the accretion disk was at its largest radial size on the decline from outburst and not peak. Further research into how the accretion disk changes with time is needed. / Department of Physics and Astronomy
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Determination of the physical parameters of the eclipsing dwarf nova system IP PegBryant, Jeffrey M. January 1998 (has links)
IP Peg is a member of a family of star systems known as cataclysmic variable stars, CVs. CVs are star systems in which a red dwarf star orbits a white dwarf and mass transfer is taking place from the red dwarf to the white dwarf. The mass ratio of the two component stars has been found the most difficult parameter to determine. Tools used in the analysis of mass-ratio included the differential photometric light curve of IP Peg, Doppler tomograms, and spectral data covering the HP emission-line. The mass ratio was found to lie in the range, q = 0.44 ± 0.14. The inclination lies in the range i = 81.5° ± 8.5°. Finally, the accretion disk radius was 0.342 times the distance between the stars. The analysis of the parameters of eclipsing CV systems like IP Peg provides a rare opportunity that helps in the understanding of other CV systems. / Department of Physics and Astronomy
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A multiwavelength analysis of the dwarf nova AR AndromedaWeindorfer, Kimberly J. January 1999 (has links)
There is no abstract available for this thesis. / Department of Physics and Astronomy
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Observational and theoretical studies on dwarf-nova outbursts / 矮新星アウトバーストについての観測的・理論的研究Kimura, Mariko 23 March 2020 (has links)
京都大学 / 0048 / 新制・課程博士 / 博士(理学) / 甲第22248号 / 理博第4562号 / 新制||理||1655(附属図書館) / 京都大学大学院理学研究科物理学・宇宙物理学専攻 / (主査)准教授 野上 大作, 教授 嶺重 慎, 教授 長田 哲也 / 学位規則第4条第1項該当 / Doctor of Science / Kyoto University / DFAM
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Fotometrický výzkum trpasličí novy EX Dra / Photometric study of dwarf nova EX DraPilarčík, Lukáš January 2011 (has links)
Photometry of eclipsing dwarf-nova EX Draconis was performed at the observatory of Astronomical Institute of the Academy of Sciences of the Czech Republic in Ondřejov and at the Astronomical Observatory on Kolonické sedlo during 63 nights. I calculated times of minimum light by two methods - the mirror method and the derivative method. The mirror method is more precise for these measurements with longer exposure time and smaller coverage of the light curve of eclipse. 53 new times of minima calculated by the mirror method and times of minima obtained from the older articles about EX Dra were included in the O-C diagram and fitted by the sine function and theoretical curve of LITE caused by an unseen third body. Period of cyclic changes for the sine function is 25 years, instead of 4 or 5 years period given in older papers.Period of the third body orbit is aproximately 17 years and its minimum mass is 53.5 Jupiter's mass. The sum of squared deviations is 5 times smaller for the LITE, which means that the LITE ilustrates the O-C diagram better. I determined the average outburst period for three observational seasons and I drew the phase curve of outburst. Finally, I calculated the short period of the light changes outside eclipse.
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ASASSN-18aan: An Eclipsing SU UMa-type Cataclysmic Variable with a 3.6-hour Orbital Period and a Late G-type Secondary Star / ASASSN-18aan: 晩期G型の伴星を伴った軌道周期3.6時間の食を起こすSU Uma型激変星Wakamatsu, Yasuyuki 23 March 2021 (has links)
京都大学 / 新制・課程博士 / 博士(理学) / 甲第23014号 / 理博第4691号 / 新制||理||1673(附属図書館) / 京都大学大学院理学研究科物理学・宇宙物理学専攻 / (主査)准教授 野上 大作, 教授 嶺重 慎, 教授 太田 耕司 / 学位規則第4条第1項該当 / Doctor of Science / Kyoto University / DFAM
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