Difference between revisions of "V 0332+53"
Kretschmar (talk | contribs) |
Kretschmar (talk | contribs) |
||
Line 66: | Line 66: | ||
= Observed pulse profiles = | = Observed pulse profiles = | ||
− | [https://ui.adsabs.harvard.edu/abs/2020A%2526A...638A.152R/abstract Alonso-Hernández et al. (2022) | + | <gallery> |
+ | File:PP_AH2022_V0332%2B53_Fig7.png|[https://ui.adsabs.harvard.edu/abs/2020A%2526A...638A.152R/abstract Alonso-Hernández et al. (2022): NuSTAR pulse profiles at different luminosities | ||
+ | File:PP_Bykov21_V0332%2B53.png | RXTE/PCA data | ||
+ | </gallery> | ||
+ | |||
+ | [https://ui.adsabs.harvard.edu/abs/2020A%2526A...638A.152R/abstract Alonso-Hernández et al. (2022)] and with different pulse types. From left to right, LX ≈ 15, 8 and 1 × 1037 erg/s, the first and last have been classified as pulse type 2, the intermediate as type 0. | ||
[[File:PP_AH2022_V0332%2B53_Fig7.png|thumb|right]] | [[File:PP_AH2022_V0332%2B53_Fig7.png|thumb|right]] | ||
[https://ui.adsabs.harvard.edu/abs/2021MNRAS.506.2156B/abstract Bykov et al. (2021)] RXTE/PCA data | [https://ui.adsabs.harvard.edu/abs/2021MNRAS.506.2156B/abstract Bykov et al. (2021)] RXTE/PCA data | ||
− | [[ | + | [[|thumb|right]] |
[https://ui.adsabs.harvard.edu/abs/2012A%26A...540A..35S/abstract Sasaki et al. (2012)] RXTE data | [https://ui.adsabs.harvard.edu/abs/2012A%26A...540A..35S/abstract Sasaki et al. (2012)] RXTE data |
Revision as of 16:10, 5 September 2023
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
[https://ui.adsabs.harvard.edu/abs/2020A%2526A...638A.152R/abstract Alonso-Hernández et al. (2022): NuSTAR pulse profiles at different luminosities
Alonso-Hernández et al. (2022) and with different pulse types. From left to right, LX ≈ 15, 8 and 1 × 1037 erg/s, the first and last have been classified as pulse type 2, the intermediate as type 0.
Bykov et al. (2021) RXTE/PCA data [[|thumb|right]]
Sasaki et al. (2012) RXTE data
Tsygankov et al. (2006) INTEGRAL JEM-X and IBIS
Zhang et al. (2005) RXTE PCA and INTEGRAL
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)