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Observational and theoretical studies on dwarf-nova outbursts

Accretion disks are ubiquitous in our universe, and produce intense brightening. How does the gas in the disk lose its angular momentum to release massive amounts of gravitational energy? This is one of the biggest open questions in astronomy. This book studies four types of newly detected outbursts...

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Bibliographic Details
Main Author: Kimura, Mariko, 1951- (Author)
Corporate Author: SpringerLink (Online service)
Format: eBook
Language:English
Published: Singapore : Springer, [2020]
Series:Springer theses.
Physical Description:
1 online resource (xxx, 179 pages) : illustrations (50 in color).
Subjects:
Online Access:SpringerLink - Click here for access

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505 0 |a Intro -- Supervisor's Foreword -- Preface -- Parts of this thesis have been published in the following journal articles: -- Contents -- List of Figures -- List of Tables -- 1 General Introduction -- 1.1 Accretion Disks in Our Universe -- 1.1.1 Gravitational Power House -- 1.1.2 Astronomical Objects with Accretion Disks -- 1.2 Dwarf Novae for the Study of Accretion Physics -- 1.3 Basic Knowledge on Cataclysmic Variables -- 1.3.1 Structure -- 1.3.2 Spectra -- 1.3.3 Evolution -- 1.4 Viscous Accretion Disks -- 1.4.1 Basic Equations -- 1.4.2 Standard Disk -- 1.5 Normal Dwarf-Nova Outbursts. 
505 8 |a 1.5.1 Discovery -- 1.5.2 Mechanism for Dwarf-Nova Outbursts -- 1.5.3 Properties of Normal Outbursts -- 1.6 Superoutbursts and Superhumps -- 1.6.1 Observations -- 1.6.2 Mechanism -- 1.6.3 Refinements in the TTI Model -- 1.6.4 WZ Sge-Type Dwarf Novae -- 1.7 Classification of Dwarf Novae -- 1.8 Tilted Accretion Disks -- 1.8.1 Discovery -- 1.8.2 Negative Superhumps -- 1.8.3 Various Observational Studies About Tilted Disks -- 1.8.4 Possible Mechanisms for Disk Tilt -- 1.8.5 Development of Warped Structures -- 1.9 Recent Progress in the Study of Dwarf Novae -- 1.9.1 Observational Tests of the TTI Model. 
505 8 |a 1.9.2 Statistically-Sophisticated Methods for Data Analyses -- 1.9.3 New Dynamical Method for Estimating Binary Mass Ratios -- 1.9.4 Discovery of a Lot of WZ Sge Stars -- 1.10 Aim of This Study -- References -- 2 Unexpected Superoutburst and Rebrightening of AL Comae Berenices in 2015 -- 2.1 Introduction -- 2.2 Observations -- 2.3 Methods for Period Analyses -- 2.4 Results -- 2.5 Discussion -- 2.5.1 Why Does AL Com Show the Shortest Interval Between Superoutbursts? -- 2.5.2 Precursor and No Early Superhumps -- 2.5.3 Same Type of Rebrightening in the Same Dwarf Nova -- 2.6 Summary -- References. 
505 8 |a 3 Outburst Properties of Possible Candidates for Period Bouncers -- 3.1 Introduction -- 3.2 Observations and Analyses -- 3.3 ASASSN-15jd -- 3.3.1 Overall Light Curve -- 3.3.2 Superhumps -- 3.4 ASASSN-16dt -- 3.4.1 Overall Light Curve -- 3.4.2 Early Superhumps -- 3.4.3 Ordinary Superhumps -- 3.5 ASASSN-16hg -- 3.5.1 Overall Light Curve -- 3.5.2 Ordinary Superhumps -- 3.6 Discussion -- 3.6.1 Mass Ratio of ASASSN-16dt Estimated by Stage a Superhumps -- 3.6.2 Luminosity Dip During the Main Superoutburst -- 3.6.3 Absence of Early Superhumps -- 3.6.4 Long Delay of Superhump Appearance. 
505 8 |a 3.6.5 Small Amplitude of Superhumps -- 3.6.6 Slow Fading Rate of Plateau Stage -- 3.7 Summary -- References -- 4 On the Nature of Long-Period Dwarf Novae with Rare and Low-Amplitude Outbursts -- 4.1 Introduction -- 4.2 Observations -- 4.2.1 Photometry -- 4.2.2 Spectroscopy -- 4.3 1SWASP J1621 -- 4.4 BD Pav -- 4.5 V364 Lib -- 4.6 Numerical Modeling of Orbital Variations -- 4.6.1 Methods -- 4.6.2 Parameters -- 4.6.3 Limitation of Our Modeling and How to Determine the Best Parameters -- 4.6.4 Results -- 4.7 Discussion -- 4.7.1 Components of the Three Objects. 
505 8 |a General introduction -- Unexpected Superoutburst and Rebrightening of AL Comae Berenices in 2015 -- Outburst Properties of Possible Candidates for Period Bouncers -- On the Nature of Long-Period DNe with Rare and Low-Amplitude Outbursts -- Thermal-viscous Instability in Tilted Accretion Disks: A Possible Application to IW And-type Dwarf Novae -- General Discussion -- Conclusions -- Appendix. 
520 |a Accretion disks are ubiquitous in our universe, and produce intense brightening. How does the gas in the disk lose its angular momentum to release massive amounts of gravitational energy? This is one of the biggest open questions in astronomy. This book studies four types of newly detected outbursts in dwarf novae through optical observations and/or numerical simulations and puts forward physical interpretations of these outbursts on the basis of the disk instability model, the most plausible model for dwarf-nova outbursts. It demonstrates that the disk-instability model can explain rich variety in dwarf-nova outbursts if some new aspects are taken into account (e.g. the extremely slow growth of tidal instability and thermal instability in the disk misaligned against the binary orbital plane). Moreover, it shares valuable insights on the evolution of binary systems by finding period bouncers and dwarf novae with F-type companion stars, which are rare objects. 
650 0 |a Dwarf novae.  |0 https://id.loc.gov/authorities/subjects/sh85040182. 
650 0 |a Accretion (Astrophysics)  |0 https://id.loc.gov/authorities/subjects/sh85000439. 
650 0 |a Cataclysmic variable stars.  |0 https://id.loc.gov/authorities/subjects/sh85020770. 
650 0 |a Stellar dynamics.  |0 https://id.loc.gov/authorities/subjects/sh94002744. 
650 6 |a Étoiles variables cataclysmiques. 
650 6 |a Dynamique stellaire. 
650 7 |a Stellar dynamics.  |2 fast. 
650 7 |a Dwarf novae.  |2 fast. 
650 7 |a Cataclysmic variable stars.  |2 fast. 
650 7 |a Accretion (Astrophysics)  |2 fast. 
650 7 |a Astronomy.  |2 fast. 
650 7 |a Astrophysics.  |2 fast. 
655 7 |a Observations.  |2 fast. 
710 2 |a SpringerLink (Online service)  |0 https://id.loc.gov/authorities/names/no2005046756. 
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