LBV 1806-20

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LBV 1806-20
1806-20 cluster.jpg
Infrared image of Cluster 1806-20. LBV 1806-20 is the brightest star, on the left.
Credit: Hubble Space Telescope
Observation data
Epoch J2000      Equinox J2000
Constellation Sagittarius
Right ascension 18h 08m 40.31s[1]
Declination −20° 24′ 41.1″[1]
Characteristics
Evolutionary stage candidate LBV[2]
Spectral type O9 - B2[2]
Apparent magnitude (J) 13.93[3]
Apparent magnitude (H) 10.75[3]
Apparent magnitude (K) 8.89[3]
Astrometry
Distance 8.7k[4] pc
Details
Mass 36[4] M
Luminosity ~2,000,000[2][5] L
Temperature 18,000–32,000[3] K
Age 3.0 – 4.5[1] Myr
Other designations
2MASS J18084031-2024411
Database references
SIMBAD data

LBV 1806-20 is a candidate luminous blue variable (LBV) and likely binary star located nearly 40,000 light-years from the Sun, towards the center of the Milky Way. It has an estimated mass of around 36 solar masses and an estimated variable luminosity of around two million times that of the Sun. It is highly luminous but is invisible from the Solar System at visual wavelengths because less than one billionth of its visible light reaches us.

When first discovered, LBV 1806-20 was considered both the most luminous and most massive star known, challenging our understanding of the formation of massive stars. Recent estimates place it somewhat nearer to Earth, which when combined with its binary nature mean that it is now well within the expected range of parameters for the most luminous stars in the galaxy.

Location[edit]

LBV 1806-20 lies at the core of radio nebula G10.0–0.3, which is believed to be primarily powered by its stellar wind.[6] It is a member of the 1806-20 open cluster, 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 four Wolf–Rayet stars, several OB stars, and a magnetar (SGR 1806-20).[4]

Spectrum[edit]

The spectral type of LBV 1806-20 is uncertain and possibly variable. It has been constrained to between O9 and B2 on the basis of an infrared HeI line equivalent width. The spectrum shows strong emission in the Paschen and Brackett series of hydrogen, but also emission lines of helium, FeII, MgII, and NaI. The lines are broad and have uneven profiles, some showing P Cygni profiles.[3] High resolution spectra show that some HeI absorption lines are doubled.[2]

Properties[edit]

Although the star is 8th magnitude at the near infrared wavelength of 2 micrometers, it is calculated to be about 35th magnitude at visible wavelengths, which is undetectable with current equipment. Intervening dust in the direction of the galactic centre absorb an estimated 29 magnitudes at visual wavelengths,[2] and so most observations are conducted using infrared telescopes.[4][1] On the basis of its luminosity and spectral type it is suspected of being an LBV, but despite the name the characteristic photometric and spectroscopic variations have not yet been observed so it remains just a candidate.[2][5]

Binary[edit]

To account for the doubled HeI lines in its spectrum and the inconsistent mass, luminosity and age estimates, LBV 1806-20 has been proposed to be a binary. The emission lines are single, so only one star appears to have a dense stellar wind as might be expected from an LBV.[2]

References[edit]

  1. ^ a b c d Figer, Donald F.; Najarro, Francisco; Geballe, T. R.; Blum, R. D.; Kudritzki, Rolf P. (2005). "Massive Stars in the SGR 1806-20 Cluster". The Astrophysical Journal. 622: L49. Bibcode:2005ApJ...622L..49F. arXiv:astro-ph/0501560Freely accessible. doi:10.1086/429159. 
  2. ^ a b c d e f g Figer, D. F.; Najarro, F.; Kudritzki, R. P. (2004). "The Double-lined Spectrum of LBV 1806-20". The Astrophysical Journal. 610 (2): L109. Bibcode:2004ApJ...610L.109F. arXiv:astro-ph/0406316Freely accessible. doi:10.1086/423306. 
  3. ^ a b c d e Eikenberry, S. S.; Matthews, K.; Lavine, J. L.; Garske, M. A.; Hu, D.; Jackson, M. A.; Patel, S. G.; Barry, D. J.; Colonno, M. R.; Houck, J. R.; Wilson, J. C.; Corbel, S.; Smith, J. D. (2004). "Infrared Observations of the Candidate LBV 1806‐20 and Nearby Cluster Stars". The Astrophysical Journal. 616: 506. Bibcode:2004ApJ...616..506E. arXiv:astro-ph/0404435Freely accessible. doi:10.1086/422180. 
  4. ^ a b c d Bibby, J. L.; Crowther, P. A.; Furness, J. P.; Clark, J. S. (2008). "A downward revision to the distance of the 1806-20 cluster and associated magnetar from Gemini Near-Infrared Spectroscopy". Monthly Notices of the Royal Astronomical Society: Letters. 386: L23. Bibcode:2008MNRAS.386L..23B. arXiv:0802.0815Freely accessible. doi:10.1111/j.1745-3933.2008.00453.x. 
  5. ^ a b Nazé, Y.; Rauw, G.; Hutsemékers, D. (2012). "The first X-ray survey of Galactic luminous blue variables". Astronomy & Astrophysics. 538: A47. Bibcode:2012A&A...538A..47N. arXiv:1111.6375Freely accessible. doi:10.1051/0004-6361/201118040. 
  6. ^ Yeung, Paul K. H.; Kong, Albert K. H.; Tam, P. H. Thomas; Lin, Lupin C. C.; Hui, C. Y.; Hu, Chin-Ping; Cheng, K. S. (2016). "Studying the SGR 1806-20/Cl* 1806-20 Region Using the Fermi Large Area Telescope". The Astrophysical Journal. 827: 41. Bibcode:2016ApJ...827...41Y. arXiv:1606.01707Freely accessible. doi:10.3847/0004-637X/827/1/41.