Winds in collision. II - an analysis of the X-ray emission from the eruptive symbiotic HM SGE

Details Winds in collision. II - an analysis of the X-ray emission from the eruptive symbiotic HM SGE Winds in collision. II - an analysis of the X-ray emission from the eruptive symbiotic HM SGE

Apr 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984a%26a...133..154w&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 133, no. 1, April 1984, p. 154-164.

Astronomy and Astrophysics

Astrophysics

57

Accretion Disks, Binary Stars, Stellar Winds, X Ray Sources, X Ray Stars, Black Body Radiation, Companion Stars, Neutron Stars, Stellar Luminosity, Stellar Spectra, White Dwarf Stars, X Ray Spectra

Scientific paper

X-ray emissions from HM Sge obtained in 1981 from the HEAO-2 satellite are analyzed and compared quantitatively with observations of HM Sge made in 1980 and of HM Sge, V 1016 Cyg, and RR Tel made in 1979. The change in the X-ray emission from HM Sge between 1979 and 1981 is found to be consistent with the X-ray luminosity and/or temperature of the emitting region declining with an e-folding timescale of the order of one to several decades. Comparison with X-ray data from V 1016 Cyg and RR Tel gives a composite X-ray light curve that is also consistent with such a decline. A comparison of the X-ray observation with spectroscopic information makes it possible to constrain the properties of the X-ray emitting region: the result is consistent with emission from an optically thin region between the two stars in the system where their winds collide head on. It is also shown that the observations are inconsistent with a stellar (blackbody) source, with emission from an accretion disk around a white dwarf or a neutron star, and with emission from a single star wind from either a white dwarf or a neutron star.

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