SS Cygni as a hard X-ray source identified with the scanning modulation collimator on HEAO 1

Details SS Cygni as a hard X-ray source identified with the scanning modulation collimator on HEAO 1 SS Cygni as a hard X-ray source identified with the scanning modulation collimator on HEAO 1

Oct 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978natur.275..721f&link_type=abstract

Nature, vol. 275, Oct. 26, 1978, p. 721-723.

Astronomy and Astrophysics

Astronomy

10

Collimators, Heao 1, Novae, Satellite-Borne Instruments, X Ray Sources, Ariel 5 Satellite, Light Curve, Radiant Flux Density, Scanners, Stellar Luminosity, Stellar Mass Accretion, Uhuru Satellite, White Dwarf Stars, X Ray Astronomy

Scientific paper

Hard X-ray emission from a 15 min by 1.5 deg area containing SS Cygni had previously been reported and identified with SS Cygni. This paper reports a 0.4 sq arc min measurement of the position of the X-ray source with the HEAO 1 modulation collimator experiment which leads to an unequivocal identification of SS Cygni as an X-ray emitter in the 2-10 keV energy range. The historical light curve in hard X-rays was also investigated by analyzing relevant Uhuru data, and two instances of possible source detection in the 2-6 keV band were noted. From Ariel 5 observations it is calculated that the X-ray luminosity of SS Cygni in the 2-10 keV energy range is of the order of 10 to the 33rd erg/sec in the optical low state and probably at least an order of magnitude less in the high state. By contrast, the soft X-ray luminosity increases by an order of magnitude between the optical low and high states. A coronal model or accretion onto the white dwarf can account for the inverse correlation of the soft and hard X-rays.

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