WR 102ea

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. Despite being a relatively unevolved star, WR 102ea has lost over half its mass already.[5]

WR 102ea
Quintuplet cluster
Cercle jaune 100%.svg
WR 102ea (circled) in the Quintuplet Cluster
Observation data
Epoch J2000      Equinox J2000
Constellation Sagittarius
Right ascension 17h 46m 15.12s[1]
Declination −28° 49′ 36.9″[1]
Characteristics
Evolutionary stage Wolf Rayet
Spectral type WN9h[2]
Apparent magnitude (K) 8.8[3]
Astrometry
Radial velocity (Rv)116[4] km/s
Proper motion (μ) RA: -0.59[1] mas/yr
Dec.: -1.21[1] mas/yr
Distance26k[2] ly
(8k[2] pc)
Details
Mass58[5] M
Radius86[2] R
Luminosity2.5 × 106[2] L
Temperature25,100[2] K
Age~4[5] Myr
Other designations
FMM 241, qF 241, (erroneously QPM-241), Q10, MGM 5-10, LHO 71
Database references
SIMBADdata

References

  1. ^ a b c d Dong, H.; Wang, Q. D.; Cotera, A.; Stolovy, S.; Morris, M. R.; Mauerhan, J.; Mills, E. A.; Schneider, G.; Calzetti, D.; Lang, C. (2011). "Hubble Space Telescope Paschen α survey of the Galactic Centre: Data reduction and products". Monthly Notices of the Royal Astronomical Society. 417: 114. arXiv:1105.1703Freely accessible. Bibcode:2011MNRAS.417..114D. doi:10.1111/j.1365-2966.2011.19013.x.
  2. ^ 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:1011.5796Freely accessible. Bibcode:2010A&A...524A..82L. doi:10.1051/0004-6361/200912612.
  3. ^ Liermann, A.; Hamann, W.-R.; Oskinova, L. M. (2009). "The Quintuplet cluster". Astronomy and Astrophysics. 494 (3): 1137. arXiv:0809.5199Freely accessible. Bibcode:2009A&A...494.1137L. doi:10.1051/0004-6361:200810371.
  4. ^ Liermann, A.; Hamann, W.-R.; Oskinova, L. M. (2009). "The Quintuplet cluster. I. A K-band spectral catalog of stellar sources". Astronomy and Astrophysics. 494 (3): 1137. arXiv:0809.5199Freely accessible. Bibcode:2009A&A...494.1137L. doi:10.1051/0004-6361:200810371.
  5. ^ a b c Liermann, Adriane; Hamann, Wolf-Rainer; Oskinova, Lidia M.; Todt, Helge (2011). "High-mass stars in the Galactic center Quintuplet cluster". Société Royale des Sciences de Liège. 80: 160. Bibcode:2011BSRSL..80..160L.

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