Abstract
Hot white dwarfs are objects that copiously emit in the Extreme Ultraviolet and soft X-ray range. They are the brightest sources seen in the Low Energy Telescope of EXOSAT. with countrates up to 25 cnts/s. in contrast to their optical and UV spectrum the totai flux and spectral distribution at soft X-ray energies are highly sensitive to the effective temperature, structure and elemental composition of the dwarf’s atmosphere. The imaging soft X-ray experiments onboard EXOSAT cover with iarge sensitivity the spectral region where the peak of emission of hot white dwarfs is expected to occur.
I here review some of the (preliminary) results obtained so far with broadband X-ray photometry on a dozen or so white dwarfs, and some of the high-resolution spectra obtained for three white dwarfs with the grating spectrometers.
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Heise, J. (1985). X-Ray Emission from Isolated Hot White Dwarfs. In: Peacock, A. (eds) X-Ray Astronomy in the Exosat Era. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-5448-9_10
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DOI: https://doi.org/10.1007/978-94-009-5448-9_10
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