V 0332+53
Also known as EXO 0331+530 and V BQ Cam Simbad [1] [2]
Monitoring Data:
RXTE/ASM Swift/BAT MAXI Fermi/GBM pulsed flux Current data in FLASHES
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.
Observed pulse profiles
Alonso-Hernández et al. (2022): NuSTAR pulse profiles at different luminosities
Bykov et al. (2021) RXTE/PCA data
Sasaki et al. (2012) RXTE data
Tsygankov et al. (2006) INTEGRAL JEM-X and IBIS
Zhang et al. (2005) RXTE PCA and INTEGRAL
Stella et al. (1985) EXOSAT
Bibliography
References
- ↑ 1.0 1.1 Tanaka, Y., 1983, IAU Circ., 3891 (NASA ADS)
- ↑ 2.0 2.1 Makishima, K., et . 1990, PASJ, 42 (NASA ADS)
- ↑ 3.0 3.1 3.2 3.3 3.4 3.5 3.6 Stella et al., 1985, ApJL, 288, L45 | http://cdsads.u-strasbg.fr/abs/1985ApJ...288L..45S
- ↑ 4.0 4.1 Pottschmidt, K., et al., 2005, ApJL 634, L97 (NASA ADS)
- ↑ Negueruela, I., Roche, P., Fabregat, J., Coe, M.J., 1999, MNRAS, 307, 695 (NASA ADS)
- ↑ Terrell, J. & Priedhorsky, W. C., ApJL, 285, L15 (NASA ADS)
- ↑ Makishima, K., Mihara, T., Ishida, M., et al., 1990, ApJ, 365, L59 (NASA ADS)