09h02m06.860s, −40° 33′ 16.91″
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| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Vela |
| Right ascension | 09h02m 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] |
| Distance | 6,600 ± 200 ly (2,020 ± 60 pc) |
| Other designations | |
Supergiant component: GP Vel, HD 77581, SAO 220767, HIP 44368, CPD−40°3072, CD−40°4838; | |
| Database references | |
| SIMBAD | data |
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]
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]
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