Observations of the peculiar hard X-ray transient X0331 + 53 (V0332 + 53)

Details Observations of the peculiar hard X-ray transient X0331 + 53 (V0332 + 53) Observations of the peculiar hard X-ray transient X0331 + 53 (V0332 + 53)

Apr 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990pasj...42..295m&link_type=abstract

Astronomical Society of Japan, Publications (ISSN 0004-6264), vol. 42, no. 2, 1990, p. 295-315.

Astronomy and Astrophysics

Astronomy

46

B Stars, Pulsars, X Ray Binaries, X Ray Sources, Annual Variations, Spaceborne Astronomy, X Ray Astronomy, X Ray Spectra

Scientific paper

Tenma observations were made of the transient 4.4-s X-ray pulsar X0331 + 53 (V0332 + 53) at several phases of its 34-d binary orbit during the period November 1983-January 1984. The measured X-ray flux and pulse periods agree with those obtained with Exosat. Rapid random fluctuations in the X-ray emission from this source were studied. It appears this type of variability is not rare among accreting pulsars, but is particularly noticeable in X0331 + 53 due to the small pulse fraction. The X-ray spectra show a turn-over above about 15 keV, which is better described by a recently introduced cyclotron absorption formula than the commonly used exponential cutoff model. In terms of this model, a magnetic field strength of about 3 x 10 to the 12th G is suggested for X0331 + 53. The absence of iron K-emission lines in the spectra indicates a rather small circumstellar matter density. This, together with the observed high luminosity (about 3 x 10 to the 36th erg/s) and large intensity modulation along the orbit, suggests that the pulsar is powered by accretion from the equatorial envelope of the supposedly Be-type primary (BQ Cam).

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