LBV 1806-20
From Wikipedia, the free encyclopedia
| Observation data Epoch J2000 |
|
|---|---|
| Constellation | Sagittarius |
| Right ascension | 18h 08m 40.3s |
| Declination | -20° 24′ 41″ |
| Apparent magnitude (V) | 35 (8.4 at 2 µm) |
| Details | |
| Mass | 130-200 M☉ |
| Radius | 150 R☉ |
| Luminosity | 5-40 × 106 L☉ |
| Temperature | 18-36,000 K |
| Metallicity | ? |
| Rotation | ? |
| Age | < 2 × 106 years |
LBV 1806-20 is a possible binary star located 30,000–49,000 light years from our Sun, toward the center of the galaxy. It has a total system mass of 130–150 Solar masses and a variable luminosity of 2 million to 40 million times that of the Sun,[1] making it comparably luminous to Eta Carinae or the Pistol Star, contenders for the most luminous star (all of which are luminous blue variables).
Despite its high luminosity, it is virtually invisible from the Solar system, because less than one billionth of its visible light reaches us, the rest being absorbed by intervening interstellar gas and dust, giving it an apparent brightness of 35th magnitude at visible wavelengths, or 8th magnitude at a near infrared wavelength of 2 micrometers.
Contents |
[edit] Formation theory
Current star formation theories tell us that a star can have at most about 120 Solar masses, but this star has been measured to have at least 130 solar masses. Some even give the star 150 to 200 solar masses.[2]
There has been some dispute as to whether LBV 1806-20 is a single star or a cluster. Its luminosity has been estimated through very high-resolution speckle imaging, the results of which suggest that LBV 1806-20 may be a single star. However, more recent high-resolution spectroscopy reveals that there may be a companion and that the mass of each star in the system could be considerably less than 130 solar masses.[3]
[edit] Location
LBV 1806-20 lies at the core of radio nebula G10.0-0.3 and is a component of cluster 1806-20, itself a component of W31, one of the largest H II regions in the Milky Way. Cluster 1806-20 is made up of some highly unusual stars, including at least two carbon-rich Wolf-Rayet stars (WC9d and WCL), two blue hypergiants, and a magnetar (SGR 1806-20).
[edit] References
- ^ Aaron Hoover (2004-01-05). Star may be biggest, brightest yet observed (English). HubbleSite. Retrieved on 2006-06-08.
- ^ Eikenberry, S.S.; Matthews, K; LaVine, J.L.; Garske, M.A.; Mu, D.; Jackson, M.A.; Patel, S.G.; Barry, D.J.; Colonno, M.R.; Houck, J. R.; Wilson, J.C; Corbel, S.; Smith, J.D. (November 2004). "Infrared Observations of the Candidate LBV 1806-20 & Nearby Cluster Stars". The Astrophysical Journal Volume 616, Issue 1: 506-518.
- ^ Figer, D.; Najarro, F.; Kudritzki, R. (August 2004). "The Double-lined Spectrum of LBV 1806-20". The Astrophysical Journal Volume 610, Issue 2: L109-L112.
