Constraints on black hole accretion in V Puppis

Abstract

In light of the recent suggestion that the nearby eclipsing binary star system V Puppis has a dark companion on a long orbit, we present the results of radio and X-ray observations of it. We find an upper limit on its radio flux of about 300 $\mu$Jy and a detection of it in the X-rays with a luminosity of about 3$\times 10^{31}$ erg/sec, a value much lower than what had been observed in some of the low angular resolution surveys of the past. These data are in good agreement with the idea that the X-ray emission from V Puppis comes from mass transfer between the two B stars in the system, but can still accommodate the idea that the X-ray emission comes from the black hole accreting stellar wind from one or both of the B stars.

3 pages, 1 figures, accepted to MNRAS

References in corpus (2)

• Refining the fundamental plane of accreting black holes
• Dependence of the orbital modulation of X-rays from 4U 1820-303 on the accretion rate