Mon. Not. R. Astron. Soc., 392, 1242-1252 (2009/January-3)
Periodicities in the high-mass X-ray binary system RXJ0146.9+6121/LSI+61°235.
SARTY G.E., KISS L.L., HUZIAK R., CATALAN L.J.J., LUCIUK D., CRAWFORD T.R., LANE D.J., PICKARD R.D., GRZYBOWSKI T.A., CLOSAS P., JOHNSTON H., BALAM D. and WU K.
Abstract (from CDS):
The high-mass X-ray binary RXJ0146.9+6121, with optical counterpart LSI+61°235 (V831Cas), is an intriguing system on the outskirts of the open cluster NGC663. It contains the slowest Be type X-ray pulsar known with a pulse period of around 1400s and, primarily from the study of variation in the emission line profile of Hα, it is known to have a Be decretion disc with a one-armed density wave period of approximately 1240d. Here we present the results of an extensive photometric campaign, supplemented with optical spectroscopy, aimed at measuring short time-scale periodicities. We find three significant periodicities in the photometric data at, in order of statistical significance, 0.34, 0.67 and 0.10d. We give arguments to support the interpretation that the 0.34 and 0.10d periods could be due to stellar oscillations of the B-type primary star and that the 0.67d period is the spin period of the Be star with a spin axis inclination of 23+10–8degrees. We measured a systemic velocity of -37.0±4.3km/s confirming that LSI+61°235 has a high probability of membership in the young cluster NGC663 from which the system's age can be estimated as 20-25Myr. From archival RXTE All Sky Monitor (ASM) data we further find `super' X-ray outbursts roughly every 450d. If these super outbursts are caused by the alignment of the compact star with the one-armed decretion disc enhancement, then the orbital period is approximately 330d.
© 2008 The Authors. Journal compilation © 2008 RAS
accretion, accretion discs - binaries: close - stars: neutron
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