V1429 Aquilae

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V1429 Aql
Observation data
Epoch J2000      Equinox J2000
Constellation Aquila[1]
Right ascension 19h 21m 33.975s[1]
Declination +14° 52′ 56.89″[1]
Apparent magnitude (V) 9.89[1]
Spectral type B3Ibe[1]
Luminosity 1,200,000 L
Temperature 25,000 K
Other designations
Database references

V1429 Aquilae is a blue hypergiant star located in the constellation of Aquila.

Physical properties[edit]

As with many other stars of its kind, V1429 Aquilae is sufficiently remote that its distance must be determined by indirect methods: estimations range between 3 and 4.3 kiloparsecs (9,800-14,000 light years),[2] with the most likely value nearer to the former, lower figure. If that is the case, then its total luminosity has been estimated to be more than 1,200,000 times that of the Sun, having a radius 60 times larguer than that of our star, and being 80 times more massive than the Sun.[3] This places it among the most luminous stars of the Milky Way. However, despite its high luminosity, it's so heavily reddened by the interstellar dust that it's totally unobservable with the naked eye and needs a telescope for its observation.[2]

V1429 Aquilae is not only a Be star but also a Luminous Blue Variable candidate due to its high luminosity[3] and later studies have shown it's actually a binary system surrounded by a disk of gas[4] as well as a very extensive bipolar nebula.[5]


  1. ^ a b c d e f "V1429 Aql". SIMBAD Astronomical Database. Retrieved 2012-12-19. 
  2. ^ a b Miroshnichenko, A. S. (August 1996). "MWC 314: a high-luminosity peculiar Be star.". Astronomy and Astrophysics 312: 941–949. Bibcode:1996A&A...312..941M. 
  3. ^ a b Miroshnichenko, A. S.; Fremat, Y.; Houziaux, L.; Andrillat, Y.; Chentson, E. L.; Klochkova, V. G. (September 1998). "High resolution spectroscopy of the galactic candidate LBV MWC 314". Astronomy and Astrophysics Supplement 312: 469–478. Bibcode:1998A&AS..131..469M. doi:10.1051/aas:1998283. 
  4. ^ Muratorio, G.; Rossi, C.; Friedjung, M. (August 2008). "Analysis of the variability of the luminous emission line star MWC 314". Astronomy and Astrophysics 487 (2): 637–644. Bibcode:2008A&A...487..637M. doi:10.1051/0004-6361:20078940. 
  5. ^ Marston, A. P.; McCollum, B. (August 2008). "Extended shells around B[e] stars. Implications for B[e] star evolution". Astronomy and Astrophysics 477 (1): 193–202. Bibcode:2008A&A...477..193M. doi:10.1051/0004-6361:20066086.