Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994pasj...46..677t&link_type=abstract
PASJ: Publications of the Astronomical Society of Japan (ISSN 0004-6264), vol. 46, no. 6, p. 677-681
Astronomy and Astrophysics
Astronomy
8
Orbital Mechanics, Stellar Flares, Stellar Mass Accretion, Stellar Orbits, X Ray Binaries, Accretion Disks, Black Holes (Astronomy), Ginga Satellite, Mass Transfer, Sky Surveys (Astronomy)
Scientific paper
An X-ray nova, GS 2023+338 (=V404 Cyg), was observed to exhibit two successive X-ray flare-ups on May 23 and May 30 in 1989 during observations with the Large Area Proportional Counter (LAC) on board the Ginga satellite. Each flare-up comprised several sporadic bursts, the intensity of which varied by a factor of 40-100 for 120-160 min. The interval of two successive flare-ups was just the orbital period of 6.5 d; both flare-ups occurred at an orbital phase of 0.294-0.311. In this case, an orbital phase of 0.0 corresponds to the superior conjunction of the compact star in the 6.5-day orbital motion of the X-ray binary. Among seven snap-shot observations with the All Sky Monitor during the early stage of the X-ray nova, one data point at an orbital phase of 0.2 on May 23 showed a high X-ray intensity of 8 count/s/cm2, whereas the others did not. These results suggest that sporadic flare-ups were likely to occur around orbital phases of 0.2-0.35 during the early stage of an X-ray nova. If so, they indicate the existence of a trigger mechanism of sporadic flare-ups which originate from the orbital motion, in addition to the mechanisms of the so-called outburst of the X-ray nova.
Egoshi Wataru
Kitamoto Shunji
Miyamoto Sigenori
Terada Kentaro
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