Comments on radial white dwarf accretion

Details Comments on radial white dwarf accretion Comments on radial white dwarf accretion

Oct 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982a%26a...114l...4k&link_type=abstract

Astronomy and Astrophysics, vol. 114, no. 1, Oct. 1982, p. L4-L6.

Astronomy and Astrophysics

Astrophysics

174

Stellar Mass Accretion, White Dwarf Stars, Coronal Loops, Electron Energy, Stellar Atmospheres, Stellar Magnetic Fields

Scientific paper

The present study of radial accretion flow onto white dwarfs for which cyclotron emission is insignificant has ascertained that conduction cannot be the dominant energy loss mechanism if a stationary, standoff shock exists above the stellar surface. It is inferred that, in such cases, an abundance of hard X-rays is emitted. By analogy with solar coronal loop models, however, conduction may lead to stellar material evaporation and subsequent enhanced bremsstrahlung losses. Conduction may therefore influence the stability and global behavior of the post-shock region. It is demonstrated that there exists a stationary bombardment solution for moderate accretion rates in which the accretion energy is transferred to the target atmosphere within one collisional mean free path, and then radiated at much lower temperatures than in the shock model. A nonstationary model without standoff shock is also proposed.

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