Difference between revisions of "V 0332+53"

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= Observed pulse profiles =
 
= Observed pulse profiles =
  
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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_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 | [https://ui.adsabs.harvard.edu/abs/2021MNRAS.506.2156B/abstract Bykov et al. (2021)] RXTE/PCA data  
 
File:PP_Bykov21_V0332%2B53.png | [https://ui.adsabs.harvard.edu/abs/2021MNRAS.506.2156B/abstract Bykov et al. (2021)] RXTE/PCA data  
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File:PP_Tsygankov2006_Fig6.png | [https://ui.adsabs.harvard.edu/abs/2006MNRAS.371...19T/abstract Tsygankov et al. (2006)] INTEGRAL JEM-X and IBIS
 
File:PP_Tsygankov2006_Fig6.png | [https://ui.adsabs.harvard.edu/abs/2006MNRAS.371...19T/abstract Tsygankov et al. (2006)] INTEGRAL JEM-X and IBIS
 
File:PP_Zhang2005_Fig3.png | [https://ui.adsabs.harvard.edu/abs/2005ApJ...630L..65Z/abstract Zhang et al. (2005)] RXTE PCA and INTEGRAL
 
File:PP_Zhang2005_Fig3.png | [https://ui.adsabs.harvard.edu/abs/2005ApJ...630L..65Z/abstract Zhang et al. (2005)] RXTE PCA and INTEGRAL
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File:PP_Stella1985_Fig1.png | [https://ui.adsabs.harvard.edu/abs/1985ApJ...288L..45S/abstract Stella et al. (1985)] EXOSAT
 
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= Bibliography =
 
= Bibliography =
 
'''References'''
 
'''References'''

Latest revision as of 23:08, 6 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

Bibliography

References

  1. 1.0 1.1 Tanaka, Y., 1983, IAU Circ., 3891 (NASA ADS)
  2. 2.0 2.1 Makishima, K., et . 1990, PASJ, 42 (NASA ADS)
  3. 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. 4.0 4.1 Pottschmidt, K., et al., 2005, ApJL 634, L97 (NASA ADS)
  5. Negueruela, I., Roche, P., Fabregat, J., Coe, M.J., 1999, MNRAS, 307, 695 (NASA ADS)
  6. Terrell, J. & Priedhorsky, W. C., ApJL, 285, L15 (NASA ADS)
  7. Makishima, K., Mihara, T., Ishida, M., et al., 1990, ApJ, 365, L59 (NASA ADS)