WR 102ea

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WR 102ea
Observation data
Epoch J2000      Equinox J2000
Constellation Sagittarius
Right ascension 17h 46m 15.12s
Declination −28° 49′ 36.9″
Characteristics
Evolutionary stage Wolf Rayet
Spectral type WN9h[1]
Apparent magnitude (K) 8.8[2]
Astrometry
Radial velocity (Rv) 116 km/s
Distance 26k[1] ly
(8k[1] pc)
Details
Mass 58[3] M
Radius 86[1] R
Luminosity 2.5 × 106[1] L
Temperature 25,100[1] K
Age probably 4 × 106 years
Other designations
FMM 241, qF 241, (erroneously QPM-241), Q10, MGM 5-10, LHO 71
Database references
SIMBAD data

WR 102ea is a Wolf–Rayet star in the Sagittarius constellation. It is the second most luminous star in the Quintuplet cluster after WR 102hb. With a luminosity of 2,500,000 times solar, it is also one of the most luminous stars known. Despite the high luminosity it can only be observed at infra-red wavelengths due to the dimming effect of intervening dust on visual light.

It is an evolved massive star which has an emission line spectrum from a strong stellar wind caused by high luminosity and the presence of elements heavier than hydrogen in the photosphere. The spectrum is dominated by ionised helium and nitrogen lines due to convectional and rotational mixing of fusion products to the surface of the star. However it is still in a core hydrogen burning phase and hydrogen lines are also visible in the spectrum, in contrast to WN stars without hydrogen which are older, less massive, and less luminous.

References[edit]

  1. ^ a b c d e f Liermann, A.; Hamann, W. -R.; Oskinova, L. M.; Todt, H.; Butler, K. (2010). "The Quintuplet cluster". Astronomy & Astrophysics 524: A82. arXiv:1011.5796. Bibcode:2010A&A...524A..82L. doi:10.1051/0004-6361/200912612.  edit
  2. ^ Liermann, A.; Hamann, W. -R.; Oskinova, L. M. (2009). "The Quintuplet cluster". Astronomy and Astrophysics 494 (3): 1137. arXiv:0809.5199. Bibcode:2009A&A...494.1137L. doi:10.1051/0004-6361:200810371.  edit
  3. ^ Adriane Liermann et all (2011). "High-mass stars in the Galactic center Quintuplet cluster". Bulletin de la Societe Royale des Sciences de Liege 80: 160-164.