V Coronae Australis

V Coronae Australis (V CrA) is a R Coronae Borealis variable star in the constellation Corona Australis. These are extremely hydrogen-deficient supergiants thought to have arisen as the result of the merger of two white dwarfs; fewer than 100 have been discovered as of 2012.[4] V Coronae Australis dimmed in brightness from 1994 to 1998.[5]

V Coronae Australis
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Corona Australis
Right ascension 18h 47m 32.31315s [1]
Declination −38° 09′ 32.3250″ [1]
Characteristics
Evolutionary stage R CrB
Astrometry
Proper motion (μ) RA: -0.90 ± 4.27[2] mas/yr
Dec.: -3.83 ± 2.81[2] mas/yr
Parallax (π)-0.39 ± 2.95[2] mas
Details
Mass0.6[3] M
Temperature6250[3] K
Other designations
V CrA, CD−38° 13089, HD 173539, HIP 92207
Database references
SIMBADdata

It has around 60% the mass of the Sun and an effective (surface) temperature of around 6250 K.[3]

ReferencesEdit

  1. ^ a b SIMBAD, V Coronae Australis (accessed 13 July 2014)
  2. ^ a b c van Leeuwen, F. (2007). "Validation of the New Hipparcos Reduction". Astronomy and Astrophysics. 474 (2): 653–64. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. S2CID 18759600.
  3. ^ a b c Stasińska, G.; Szczerba, R.; Schmidt, M.; Siódmiak, N. (2006). "Post-AGB stars as testbeds of nucleosynthesis in AGB stars". Astronomy and Astrophysics. 450 (2): 701. arXiv:astro-ph/0601504. Bibcode:2006A&A...450..701S. doi:10.1051/0004-6361:20053553. S2CID 12040452.
  4. ^ Tisserand; Clayton; Welch; Pilecki; Wyrzykowski; Kilkenny (2012). "The Ongoing Pursuit of R Coronae Borealis Stars: ASAS-3 Survey Strikes Again". Astronomy & Astrophysics. 551: 22. arXiv:1211.2475. Bibcode:2013A&A...551A..77T. doi:10.1051/0004-6361/201220713. S2CID 59060842. A77.
  5. ^ Skuljan, L.; Cottrell, P. L. (2002). "Recent declines of RS Telescopii, UW Centauri, and V Coronae Australis". The Observatory. 122: 322–29. Bibcode:2002Obs...122..322S.