The Mir/Kvant team detected renewed strong X-ray emission on 1995 February 16 ( Borozdin, Alexandrovich, & Sunyaev 1995). Because of the timescale of its initial outburst in 1993, it is also called an X-ray nova. Della Valle, Mirabel, & Rodríguez (1994) used these data to argue that the source is a low-mass binary 2 3 kpc from the Sun.
The optical and radio counterparts were detected by Della Valle, Mirabel, & Cordier (1993) and Mirabel, Rodríguez, & Cordier (1993). 1993), and with BATSE, on the Compton Gamma Ray Observatory ( Harmon et al. The hard X-ray transient GRS 1716-249 was first discovered with SIGMA, on Granat ( Ballet et al. Subject headings: black hole physics radio continuum: stars stars: individual (Nova Ophiuchi 1993, GRS 1716-249) X-rays: stars This strengthens the apparent empirical link between changes in accretion disk X-ray emission and radio activity in galactic black hole binaries. Although the X-ray flares, as seen at 20 200 keV by BATSE, are unusual in having sawtooth-like, slow-rise, fast-decay time profiles, the relation between X-ray and radio events is similar to that in the superluminal radio jet X-ray transient GRO J1655-40. Radio observations by the Molonglo Observatory Synthesis Telescope and the Very Large Array show a rapidly decaying radio flare followed by recurrent radio flaring activity. The X-ray Nova Ophiuchi 1993, GRS 1716-249 (=GRO J1719-24), discovered in 1993 September, was redetected as an X-ray source by the Mir/Kvant team on 1995 February 16, and later by BATSE.
M CK AY CSIRO Australia Telescope, Paul Wild Observatory, Narrabri, NSW 2390, Australia Received 1996 June 17 accepted 1996 August 7 H UNSTEAD School of Physics, University of Sydney, Sydney, NSW 2006, Australia AND D. S HRADER Laboratory for High Energy Astrophysics, NASA Goddard Space Flight Center, Greenbelt MD 20771 D. R UPEN National Radio Astronomy Observatory, P.O. Radio and X-Ray Flaring Events in X-Ray Nova Ophiuchi 1993 R. Flaring Events in X-Ray Nova OPH 1993 T HE A STROPHYSICAL J OURNAL, 470:L105 L107, 1996 October 20
0 kommentar(er)
