Vela X-1

This article is about the high-mass X-ray binary system. For pulsar associated with the Vela supernova remnant, see Vela Pulsar.
Vela X-1

A visual band light curve for GP Velorum, adapted from Tjemkes et al. (1986)[1]
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Vela
Right ascension 09h 02m 06.861s[2]
Declination −40° 33′ 16.90″[2]
Apparent magnitude (V) 6.87
Characteristics
Spectral type B0.5Ia
Apparent magnitude (B) 7.301
Apparent magnitude (V) 6.926
Apparent magnitude (J) 5.833±0.020
Apparent magnitude (H) 5.705±0.034
Apparent magnitude (K) 5.596±0.024
U−B color index −0.51[3]
B−V color index 0.50[3]
Variable type Complex[citation needed]
Astrometry
Proper motion (μ) RA: −4.822[2] mas/yr
Dec.: 9.282[2] mas/yr
Parallax (π)0.4962 ± 0.0152 mas[2]
Distance6,600 ± 200 ly
(2,020 ± 60 pc)
Other designations
Supergiant component: GP Vel, HD 77581, SAO 220767, HIP 44368, CPD−40°3072, CD−40°4838;
X-ray component: 1XRS 09002-403, 1RXS J090207.0-403311, 4U 0900-40
Database references
SIMBADdata

Vela X-1 is a pulsing, eclipsing high-mass X-ray binary (HMXB) system, associated with the Uhuru source 4U 0900-40 and the supergiant star HD 77581. The X-ray emission of the neutron star is caused by the capture and accretion of matter from the stellar wind of the supergiant companion. Vela X-1 is the prototypical detached HMXB.[4]

The orbital period of the system is 8.964 days, with the neutron star being eclipsed for about two days of each orbit by HD 77581. It has been given the variable star designation GP Velorum, and it varies from visual magnitude 6.76 to 6.99.[5] The spin period of the neutron star is about 283 seconds, and gives rise to strong X-ray pulsations. The mass of the pulsar is estimated to be at least 1.88±0.13 solar masses.[6]

Characteristics

Long term monitoring of the spin period shows small random increases and decreases over time similar to a random walk.[7] The accreting matter causes the random spin period changes. However, a recent study has detected nearly periodic spin period reversals in Vela X-1 on long time-scales of about 5.9 years.[8]

See also

References

  1. ^ Tjemkes, S. A.; Zuiderwijk, E. J.; van Paradijs, J. (January 1986). "Optical light curves of massive X-ray binaries". Astronomy and Astrophysics. 154: 77–91. Bibcode:1986A&A...154...77T. Retrieved 29 April 2022.
  2. ^ a b c d e Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
  3. ^ a b Klare, G.; Neckel, T. (1977). "UBV, Hβ and polarization measurements of 1660 southern OB stars". Astronomy and Astrophysics Supplement. 27: 215. Bibcode:1977A&AS...27..215K.
  4. ^ Mauche, C. W.; Liedahl, D. A.; Akiyama, S.; Plewa, T. (2007). "Hydrodynamic and Spectral Simulations of HMXB Winds". Progress of Theoretical Physics Supplement. 169: 196–199. arXiv:0704.0237. Bibcode:2007PThPS.169..196M. doi:10.1143/PTPS.169.196. S2CID 17149878.
  5. ^ "GP Vel". International Variable Star Index. AAVSO. Retrieved 29 April 2022.
  6. ^ Quaintrell, H.; et al. (2003). "The mass of the neutron star in Vela X-1 and tidally induced non-radial oscillations in GP Vel". Astronomy and Astrophysics. 401: 313–324. arXiv:astro-ph/0301243. Bibcode:2003A&A...401..313Q. doi:10.1051/0004-6361:20030120. S2CID 5602110.
  7. ^ Bildsten, L.; et al. (1997). "Observations of Accreting Pulsars". The Astrophysical Journal Supplement Series. 113 (2): 367–408. arXiv:astro-ph/9707125. Bibcode:1997ApJS..113..367B. doi:10.1086/313060. S2CID 706199.
  8. ^ Chandra, A. D.; et al. (2021). "Detection of nearly periodic spin period reversals in Vela X-1 on long time-scales: inkling of solar-like cycle in the donor star?". Monthly Notices of the Royal Astronomical Society. 508 (3): 4429–4442. arXiv:2108.07097. Bibcode:2021MNRAS.508.4429C. doi:10.1093/mnras/stab2382.