Gravitational Collapse of Mass-Accreting White Dwarfs
نویسندگان
چکیده
منابع مشابه
Accreting White Dwarfs
Thermonuclear (type Ia) supernovae are explosions in accreting white dwarfs, but the exact scenario leading to these explosions is still unclear. An important step to clarify this point is to understand the behaviour of accreting white dwarfs in close binary systems. The characteristics of the white dwarf (mass, chemical composition, luminosity), the accreted material (chemical composition) and...
متن کاملInternal Conditions of Accreting White Dwarfs
We explain the physics of compressional heating of the deep interior of an accreting white dwarf (WD) at accretion rates low enough so that the accumulated hydrogen burns unstably and initiates a classical nova (CN). In this limit, the WD core temperature (Tc) reaches an equilibrium value (Tc,eq) after accreting an amount of mass much less than the WD’s mass. Once this equilibrium is reached, t...
متن کاملPulsational Instabilities in Accreting White Dwarfs
The Cataclysmic Variable (CV) population harbors a diverse range of donor stars and accreting white dwarfs (WDs). A range of WD masses is expected, from low mass Helium core WDs, to massive WDs which have previously accreted at rates high enough for Hydrogen to burn steadily. Furthermore, a wide range of Helium enrichment is expected in the accreted material depending on the degree to which the...
متن کاملMagnetic Field Evolution in Accreting White Dwarfs
We discuss the evolution of the magnetic field of an accreting white dwarf. We calculate the ohmic decay modes for accreting white dwarfs, whose interiors are maintained in a liquid state by compressional heating. We show that the lowest order ohmic decay time is (8–12) billion years for a dipole field, and (4–6) billion years for a quadrupole field. We then compare the timescales for ohmic dif...
متن کاملCompressional Heating of Accreting White Dwarfs in CV’s
In recent years several Dwarf Novae (DN) systems have been observed in quiescence, when the accretion rate is low and the WD photosphere can be directly detected. The WDs are observed to cool after the DN outburst from high effective temperatures to lower effective temperatures (Teff) thought to be indicative of the thermal state of the deep interior of the WD. Sion has argued that the most lik...
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ژورنال
عنوان ژورنال: International Astronomical Union Colloquium
سال: 1989
ISSN: 0252-9211
DOI: 10.1017/s0252921100099346