LBV 1806-20
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Stern LBV 1806-20 |
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| Comparison between LBV 1806-20 and the sun (computer graphics) | |
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Observation dates equinox : J2000.0 , epoch : J2000.0 |
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| Constellation | Sagittarius |
| Right ascension | 18 h 08 m 40.3 s |
| declination | −20 ° 24 ′ 41 ″ |
| Apparent brightness | about 35 mag |
| Typing | |
| Astrometry | |
| distance | 30,000–49,000 ly |
| Physical Properties | |
| Dimensions | 130-200 M ☉ |
| radius | approx. 150 R ☉ |
| Luminosity |
2,000,000–40,000,000 L ☉ |
| Effective temperature | 18,000 - 36,000 K. |
| Age | ≈ 2,000,000 a |
The name LBV 1806-20 stands for one of the most massive binary star systems in the Milky Way that has been discovered so far. It is located between 30,000 and 49,000 light years from the solar system towards the galactic center.
The discovery was announced in January 2004 by astronomers at the University of Florida . However, between LBV 1806-20 and our solar system there are accumulations of gas and dust that absorb its light. We can therefore only perceive the star in the infrared range.
In 2008, a double line spectrum at LBV 1806-20 and the mass of the binary star system were calculated as 130 solar masses with a luminosity of 1,000,000 solar luminosities. At least one component of the binary star system is a variable star of the class Luminous Blue Variables , LBV for short, such as Eta Carinae .
Individual evidence
- ^ Donald F. Figer, Francisco Najarro, Rolf P. Kudritzki: THE DOUBLE-LINED SPECTRUM OF LBV 1806-20 . In: Astrophysics. Solar and Stellar Astrophysics . 2008, arxiv : astro-ph / 0406316v1 .