Astronomy and Astrophysics – Astronomy
Scientific paper
May 1979
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979phdt.........5d&link_type=abstract
Ph.D. Thesis California Inst. of Tech., Pasadena.
Astronomy and Astrophysics
Astronomy
Dwarf Stars, Luminous Intensity, Novae, Stellar Mass Accretion, X Ray Astronomy, Black Body Radiation, Heao 1, Pulsed Radiation, Radiant Flux Density, Stellar Luminosity
Scientific paper
The detection by HEAO-1 of pulsed soft X-rays (0.1 - 0.5 keV) with a period of 9 s and a pulsed fraction that varies between 0 and 100% from SS Cygni at the peak of an optical outburst confirms for the first time the supposed high-energy origin of the optical pulsations seen from dwarf novae. The pulse shape is remarkably sinusoidal for such a large amplitude oscillation. A soft X-ray pulsation detected from U Geminorum on the declining portion of an optical outburst is quasi-periodic with periods ranging from 20 to 30 s, and present throughout all binary phases with an average amplitude of approximately 15%. A preliminary survey of the soft X-ray emission from approximately 65 dwarf novae during quiescence was also made. Thus far, soft X-rays were detected only at positions coincident with those of AY Lyrae and EX Hydrae. The quiescent state spectra of dwarf novae are compared with their outburst spectra. It is concluded that variations in the mass accretion rate may account for the variety of X-ray behavior observed.
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