BI 253
| Observation data Epoch J2000 Equinox J2000 |
|
|---|---|
| Constellation | Dorado |
| Right ascension | 05h 37m 34.461s[1] |
| Declination | −69° 01′ 10.20″[1] |
| Apparent magnitude (V) | 13.76[2] |
| Characteristics | |
| Evolutionary stage | Main sequence[3] |
| Spectral type | O2V-III(n)((f*))[3] |
| U−B color index | −1.02[4] |
| B−V color index | −0.13[4] |
| Astrometry | |
| Proper motion (μ) | RA: 2.3[1] mas/yr Dec.: 3.1[1] mas/yr |
| Distance | 164,000 ly (50,000[5] pc) |
| Absolute magnitude (MV) | −5.7[3] |
| Details | |
| Mass | 84[3] M☉ |
| Radius | 10.7[2] R☉ |
| Luminosity | 912,000[3] L☉ |
| Surface gravity (log g) | 4.20[2] cgs |
| Temperature | 50,100[3] K |
| Rotational velocity (v sin i) | 200[3] km/s |
| Other designations | |
| Database references | |
| SIMBAD | data |
BI 253 is an O2V star in the Large Magellanic Cloud and is a primary standard of the O2 type. It is one of the hottest main-sequence stars known and one of the most-massive and most-luminous stars known.
Discovery
BI 253 was first catalogued in 1975 as the 253rd of 272 likely O and early B stars in the Large Magellanic Cloud.[4] In 1995, the spectral type was analysed to be O3 V, the earliest type defined at that time.[6]
When the classification of the earliest type O stars was refined in 2002, the complete lack of neutral helium or doubly ionised nitrogen lines in the spectrum led to BI 253 being placed in a new O2 V class. It was given a ((f*)) qualifier because of the very weak emission lines of helium and nitrogen.[7] The most recent published data gives a spectral type of O2V-III(n)((f*)), although it is unclear whether this is due to higher quality spectra or an actual change in the spectrum.[3][8]
BI 253 has been proposed as a runaway star because of its relatively isolated position outside the main star-forming areas of 30 Doradus. However, it does not exhibit a particularly high space velocity or any other indicators such as a bow shock.[9][10]
Properties
BI 253 is one of the hottest, most massive, and most luminous known main sequence stars.[11] The temperature is around 50,000 K, the luminosity over 750,000 L☉, and the mass over 80 M☉, although it is less than 11 R☉. The rotation rate of at least 200 km/s is high, but this is common in the youngest and hottest stars, either due to spin-up during stellar formation or merger of a close binary system.
Evolution
BI 253 is still burning hydrogen in its core, but shows enrichment of nitrogen and helium at the surface due to strong rotational and convectional mixing and because of its strong stellar wind. It is very close to the expected ZAMS position for an 85 M☉ star. It is expected that stars more massive than BI 253 would show a giant or supergiant luminosity class even on the main sequence.[11]
See also
References
- ↑ 1.0 1.1 1.2 1.3 Lua error in package.lua at line 80: module 'strict' not found.
- ↑ 2.0 2.1 2.2 Lua error in package.lua at line 80: module 'strict' not found.
- ↑ 3.0 3.1 3.2 3.3 3.4 3.5 3.6 3.7 Lua error in package.lua at line 80: module 'strict' not found.
- ↑ 4.0 4.1 4.2 Lua error in package.lua at line 80: module 'strict' not found.
- ↑ Lua error in package.lua at line 80: module 'strict' not found.
- ↑ Lua error in package.lua at line 80: module 'strict' not found.
- ↑ Lua error in package.lua at line 80: module 'strict' not found.
- ↑ Lua error in package.lua at line 80: module 'strict' not found.
- ↑ Lua error in package.lua at line 80: module 'strict' not found.
- ↑ Lua error in package.lua at line 80: module 'strict' not found.
- ↑ 11.0 11.1 Lua error in package.lua at line 80: module 'strict' not found.
