![]() We show that, while models that allow only for X-ray heating can explain the observed intensities of the Balmer lines, they cannot, at the same time, explain the intensities of the He i and He ii lines in the optical spectra. The calculations determine self-consistently the thermal structure of the funnel, allowing for radiative transfer, electron scattering and the trapping of radiation within the funnel, and represent a substantial improvement on previous purely kinematical models. We present calculations of the thermal structure of accretion funnels heated by hard X-ray emission from the accretion shock, soft X-ray reprocessed radiation from the white dwarf surface and magnetic heating in the matter–field interaction region close to the orbital plane.
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