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Star system in the constellation Carina From Wikipedia, the free encyclopedia
HD 93205, or V560 Carinae, is a binary stellar system, in the Carina Nebula (NGC 3372) in the constellation Carina. It consists of two massive O-stars that revolve around each other in 6 days.
 | |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Carina |
| Right ascension | 10h 44m 33.739s[1] |
| Declination | −59° 44′ 15.43″[1] |
| Apparent magnitude (V) | 7.75[2] |
| Characteristics | |
| Spectral type | O3.5Vf + O8V[3] |
| U−B color index | −0.91[2] |
| B−V color index | +0.05[2] |
| Variable type | Ellipsoidal[4] |
| Astrometry | |
| Radial velocity (Rv) | 3.6 km/s |
| Proper motion (μ) | RA: −6.619[1] mas/yr Dec.: 2.947[1] mas/yr |
| Parallax (π) | 0.4308 ± 0.0248 mas[1] |
| Distance | 7,600 ± 400 ly (2,300 ± 100 pc) |
| Absolute magnitude (MV) | −5.87 + −4.32[5] |
| Orbit[6] | |
| Period (P) | 6.0803 days |
| Eccentricity (e) | 0.370 |
| Inclination (i) | 60[7]° |
| Semi-amplitude (K1) (primary) | 132.6 km/s |
| Semi-amplitude (K2) (secondary) | 313.6 km/s |
| Details | |
| Mass | 40 - 60[6] M☉ |
| Radius | 9.2[7] R☉ |
| Luminosity | 1,160,000[5] L☉ |
| Temperature | 51,300[5] K |
| secondary | |
| Mass | 17 - 25.3[6] M☉ |
| Radius | 7.0[7] R☉ |
| Luminosity | 112,000[5] L☉ |
| Temperature | 38,000[5] K |
| Age | < 2[6] Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
The more massive member of the pair is an O3.5 main sequence star. The spectrum shows some ionised nitrogen and helium emission lines, indicating some mixing of fusion products to the surface and a strong stellar wind. The mass calculated from apsidal motion of the orbits is 40 to 60 M☉. This is somewhat lower than expected from evolutionary modelling of a star with its observed parameters.[6]
The less massive member is an O8 main sequence star of approximately 20 M☉.[7] It moves in its orbit at a speed of over 300 km/s and is considered to be a relativistic binary, which causes the apses of the orbit to change in a predictable way.[5]
The closeness of the two stars causes them to become deformed, and this means that the observed brightness of the system varies slightly every six days during its orbit. The total amplitude of the variation is only 0.02 magnitudes.[4]
It is generally considered as a member of the open cluster Trumpler 16.[9] Among its neighbors are some of the most massive and luminous stars in the galaxy, like Eta Carinae, HD 93250 and the binary WR 25. It lies five arc-minutes from Eta Carinae.
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