Accreting white dwarfs :from exoplanetary probes to classical novae and Type 1a supernovae /

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"Version: 20230901"--Title page verso.Includes bibliographical references.1. A brief introduction to the physics of non-accreting white dwarfs -- 1.1. A historical background of the study of white dwarfs -- 1.2. Electron degeneracy -- 1.3. The inverse relation between WD mass and radius -- 1.4. The Chandrasekhar limit -- 1.5. Core compositions versus WD mass -- 1.6. Cooling evolution -- 1.7. WD atmospheres and envelope compositions -- 1.8. Gravitational and thermal diffusion -- 1.9. Radiative acceleration -- 1.10. Convective mixing and dredge-up -- 1.11. Rotational velocities of non-accreting isolated WDs2. Accretion of interstellar gas and dust by white dwarfs -- 2.1. Early spectroscopic observations of Photospheric metals in cool white dwarfs -- 2.2. Interstellar gas and dust accretion as the external source of metals -- 2.3. The two-phase ISM accretion model of Dupuis, Fontaine and Wesemael -- 2.4. Comparison of white dwarf kinematics with maps of the local ISM -- 2.5. The demise of ISM accretion as the source of metals in cool white dwarfs3. Accreting white dwarfs as probes of the formation, composition and evolution of exoplanetary systems -- 3.1. Introduction to exoplanetary debris accretion onto white dwarfs -- 3.2. WD accretion of tidally disrupted asteroids -- 3.3. Comet accretion onto a WD -- 3.4. Does accretion by ISM or detached DA + dM binaries still have a role? -- 3.5. Disk structure and accretion rates onto WDs -- 3.6. Gaseous disks -- 3.7. Accretion rates -- 3.8. Diffusion in WDs accreting exoplanetary matter -- 3.9. Spectroscopic abundances and the chemical composition of exoplanetary matter accreted by WDs -- 3.10. Summary4. Accreting WDs in Roche Lobe-detached post-common envelope main sequence-white dwarf binaries -- 4.1. Mass loss rates from late-type dwarfs in PCEBs -- 4.2. Characterizing the population of main sequence-WD PCEBs -- 4.3. Accretion of outflows from detached main sequence dwarfs onto WDs in PCEBs -- 4.4. The ever-changing saga of the hot DAZ.9 WD in the PCEB Feige 24 -- 4.5. Beyond Feige 24 : the case for accretion of M dwarf winds onto non-magnetic WDs in PCEBs -- 4.6. Accretion onto magnetic WDs in PCEBs -- 4.7. V471 Tauri, the king of accreting magnetic PCEBs -- 4.8. Low-accretion rate polars (LARPS) and pre-polars (PREPS) -- 4.9. Webbink and Wickramasinghe (2005) magnetic siphon -- 4.10. what is the origin of the high field magnetic degenerates?5. accreting white dwarfs in symbiotic variable binaries -- 5.1. introduction -- 5.2. theoretical studies of the wind accretion in symbiotics -- 5.3. the outbursts of symbiotic variables6. accreting white dwarfs in the helium-rich AM Canum Venaticorum systems -- 6.1. Introduction -- 6.2. Characterizing the observed behavior of AM CV systems -- 6.3. Theoretical interpretation of the observed behavior of AM CVn outbursts -- 6.4. The formation of AM CVn binaries -- 6.5. The masses, effective temperatures, chemical abundances and rotational velocities of accreting WDs in AM CVn binaries -- 6.6. Masses of AM CVn accreting WDs -- 6.7. The heating and cooling of accreting WDs in AM CVn systems -- 6.8. Conclusion7. The accreting white dwarfs in cataclysmic variables -- 7.1. Introduction to accreting white dwarfs in cataclysmic variables -- 7.2. CV white dwarf masses -- 7.3. Masses of the accreting magnetic white dwarfs in polars and intermediate polars -- 7.4. CV white dwarf temperatures -- 7.5. Rotational velocities of CV white dwarfs -- 7.6. Chemical abundances in CV WD photospheres -- 7.7. CV WD second flux components and boundary layer structure : a mystery -- 7.8. Accreting pulsating CV WDs -- 7.9. A new era in research on cataclysmic variable accreting WDs -- 7.10. Structure, evolution, heating and cooling of CV WDs -- 7.11. Classical novae, recurrent novae, symbiotic variables : the single degenerate pathway to supernovae Type Ia?The astrophysical process of accretion onto compact central objects is ubiquitous across the universe. The study of white dwarf stars has greatly expanded in recent years, and this book presents, from first principles, the physics of the accretion process onto white dwarfs. Among the resulting phenomena are isolated white dwarfs accreting interstellar gas and dust as they orbit the galactic center, white dwarfs accreting from the debris disks of tidally disrupted asteroids, comets and exoplanets in other exoplanetary systems, white dwarfs accreting from red giant winds in symbiotic variable stars, white dwarfs accreting from Roche lobe-detached main sequence stars, white dwarfs accreting in cataclysmic variables, helium accreting white dwarfs in the ultra-compact AM CVn binaries, accreting white dwarf explosions in classical novae and Type Ia supernovae, the cosmologically critical white dwarf supernovae that led to the discovery of the accelerating expansion of the universe and the existence of dark energy. This book is intended for advanced undergraduates, graduate students, astrophysicists who specialize in white dwarf studies as well as non-specialist scientists.Senior undergraduate and graduate students, researchers in stellar astrophysics.Also available in print.Mode of access: World Wide Web.System requirements: Adobe Acrobat Reader, EPUB reader, or Kindle reader.Edward M. Sion is Professor in the Department of Astrophysics and Planetary Science at Villanova University and a leading expert in the field. He specializes on the structure and evolution of white dwarf stars and white dwarf stars in explosive binary star systems known as cataclysmic variables. His primary research interests include the formation and evolution of white dwarf stars, the physics and evolution of cataclysmic variable stars, and theoretical studies of accretion physics.Title from PDF title page (viewed on October 3, 2023).

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: .,

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1 online resource (various pagings) :illustrations (some color).

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English

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9780750320429

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523.8

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Subject(s)

Galaxies & stars.
SCIENCE / Space Science / Astronomy.
White dwarf stars.
Accretion (Astrophysics)

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Edward M Sion.

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