V 0332+53
Revision as of 13:54, 18 April 2018 by Kuehnel (talk | contribs) (Created page with "Category:Accreting X-ray Pulsars Also known as EXO 0331+530 and V BQ Cam [http://simbad.u-strasbg.fr/simbad/sim-id?Ident=V0332%2B53&NbIdent=1&Radius=2&Radius.unit=arcmin&...")
Also known as EXO 0331+530 and V BQ Cam Simbad [1] [2]
Monitoring Data:
RXTE/ASM Swift/BAT MAXI Fermi/GBM pulsed flux
System Overview
| Porb | 34.25 | days | [3] |
| Pspin | ~4.4 | s | [3] |
| B | 2.7 x 1012 | G | [4] |
| a sin i | 48±4 | lt-sec | [3] |
| eccentricity | 0.31±0.03 | [3] | |
| ω | 313±10 | degree | [3] |
| Τperiastron | 2445652±1 | JD | [3] |
| distance | ~7 | kpc | [5] |
Description
V 0332+53 was first recognized in Tenma observations from late 1983 to January 1984 ([1], [2]). After the detection it was realized that it had been seen by Vela 5B in 1973 ([6]). Follow-up observations by EXOSAT discovered pulsations and allowed the determination of orbital parameters ([3]).
The Tenma observations already showed evidence for a cyclotron line at ~28 keV. Ginga observations (2–60 keV) during an outburst in 1989 found two lines at 28.5 and 53 keV ([7]). During the next bright outburst in 2004, INTEGRAL observations ([4]) found a third cyclotron line at ~74 keV.
References
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