NGC 2363-V1
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 The H II region NGC 2363 as seen by the Hubble Space Telescope. The green arrow points to NGC 2363-V1.[1] Credit: NASA/ESA | |
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Camelopardalis[2] |
| 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[3] pc) |
| Absolute magnitude (MV) | −10.25[1] |
| Details | |
| Mass | ~20[4] M☉ |
| Radius | 194 – 356[5] R☉ |
| Luminosity (bolometric) | ≤790,000 – 6,310,000[5] L☉ |
| Temperature | 13,500 - 26,000[5] K |
| Metallicity [Fe/H] | −1 – −0.6[3] dex |
| Age | 4-5[6] Myr |
| Database references | |
| SIMBAD | data |
NGC 2363-V1 is a luminous blue variable star in the star-forming region NGC 2363, at the far southwestern part of the irregular galaxy NGC 2366 in the constellation Camelopardalis, near the north celestial pole nearly 11 million light years away from our galaxy. It was discovered in 1996 by Laurent Drissen, Jean-René Roy, and Carmelle Robert while examining images taken by the Hubble Space Telescope Wide 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 to P Cygni rather than the presently cool Eta Carinae outburst spectrum.[1][3]
