Eta Centauri
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| Observation data Epoch J2000 |
|
|---|---|
| Constellation | Centaurus |
| Right ascension | 14h35m30.4s |
| Declination | −42°09′28″ |
| Apparent magnitude (V) | +2.33 |
| Spectral Characteristics | |
| Spectral type | B1.5Vne |
| U-B color index | −0.83 |
| B-V color index | −0.19 |
| Variable type | Gamma Cas |
| Astrometry | |
| Radial velocity (Rv) | 0 km/s |
| Proper motion (μ) | RA: −35.31 mas/yr Dec.: −32.44 mas/yr |
| Parallax (π) | 10.57 ± 0.83 mas |
| Distance | 310 ± 20 ly (95 ± 7 pc) |
| Absolute magnitude (MV) | −2.54 |
| Physical Characteristics | |
| Mass | 8.5-10.5 M☉ |
| Radius | 5-6 R☉ |
| Luminosity | 6,000 L☉ |
| Temperature | 20,000 K |
| Metallicity | ? |
| Rotation | 333 km/s. |
| Age | < 2 × 107 years |
| Other designations | |
| Database references | |
| SIMBAD | data |
Eta Centauri (η Cen / η Centauri) is a star in the constellation Centaurus.
This is a rapidly rotating star that completes a full rotation in less than a day. It is also a Be star, which means it has variable emissions in its hydrogen spectral lines. Finally it is also slightly variable, and classified as a Gamma Cassiopeiae variable, with multiple periods of variability. It is approximately 309 light years from Earth. Eta Centauri is sufficiently large that it is on the dividing line between stars that evolve into white dwarfs and those that turn into a supernovae.
[edit] References
- Janot-Pacheco, E. et al, (1999). "Multi-periodicity of the Be star η Centauri from spectroscopic and photometric observations". A&AS 137: 407.
[edit] External links
- Eta Centauri by Jim Kaler.
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