 TheH II region NGC 2363 as seen by theHubble Space Telescope. The green arrow points to NGC 2363-V1.[1] Credit:NASA/ESA | |
| Observation data EpochJ2000.0 EquinoxJ2000.0 | |
|---|---|
| Constellation | Camelopardalis |
| Right ascension | 07h 28m 43.37s[1] |
| Declination | +69° 11′ 23.9″[1] |
| Apparent magnitude (V) | 17.88[1] |
| Characteristics | |
| Evolutionary stage | LBV |
| Spectral type | LBV |
| Variable type | LBV |
| Astrometry | |
| Distance | 10,800,000 ly (3,300,000[2] pc) |
| Absolute magnitude (MV) | −10.25[1] |
| Details | |
| Mass | ~20[3] M☉ |
| Radius | 194 – 356[4] R☉ |
| Luminosity (bolometric) | ≤790,000 – 6,310,000[4] L☉ |
| Temperature | 13,500 - 26,000[4] K |
| Metallicity [Fe/H] | −1 – −0.6[2] dex |
| Age | 4-5[5] Myr |
| Database references | |
| SIMBAD | data |
NGC 2363-V1 is aluminous blue variable star in the star-forming regionNGC 2363, at the far southwestern part of theirregular galaxyNGC 2366 in theconstellationCamelopardalis, near thenorth celestial pole nearly 11 millionlight years away from our galaxy. It was discovered in 1996 by Laurent Drissen, Jean-René Roy, andCarmelle Robert while examining images taken by theHubble Space TelescopeWide Field Planetary Camera 2.[1]
NGC 2363-V1 is one of the most luminous stars known. It has been undergoing an increase in temperature and luminosity for the last 20 years, after a dramatic increase in its rate of mass loss. Significant luminosity variation within a human lifetime is rare in LBVs, e.g.Eta Carinae during its Great Eruption (1837 to 1855). NGC 2363-V1 shows an extreme B hypergiant spectrum similar toP Cygni rather than the presently cool Eta Carinae outburst spectrum.[1][2]
