X-ray Emission from Accretion on to White Dwarfs
Open Access
- 1 April 1976
- journal article
- research article
- Published by Oxford University Press (OUP) in Monthly Notices of the Royal Astronomical Society
- Vol. 175 (1) , 43-60
- https://doi.org/10.1093/mnras/175.1.43
Abstract
We have extended calculations by Hoshi and by Aizu to produce a self-consistent model for X-radiation from accreting, possibly magnetized, white dwarfs. To generate keV X-rays the flow must be radial on to the stellar surface. We expect X-ray luminosities to be in the range |${10}^{32}-{10}^{36}\,\text{erg}\,\text{s}^{-1}$|, and the spectra to be quasi-bremsstrahlung with |$kT\,\sim \,30-100\,\text{keV}$| and with a substantial low energy cut-off. The optical (bolometric) luminosity should be comparable to that emitted in the X-rays. If the white dwarf is magnetized a comparable, or greater, amount can be radiated as cyclotron emission in the infrared or optical.Keywords
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