V Coronae Australis (V CrA) is a R Coronae Borealis variable (RCB) 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.[9] V Coronae Australis dimmed in brightness from 1994 to 1998.[10]
Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
---|---|
Constellation | Corona Australis |
Right ascension | 18h 47m 32.30962s[2] |
Declination | −38° 09′ 32.3079″[2] |
Apparent magnitude (V) | 9.4 - 17.9[3] |
Characteristics | |
Evolutionary stage | R CrB[3] |
Spectral type | R0[4] |
Astrometry | |
Proper motion (μ) | RA: −1.104[2] mas/yr Dec.: −7.531[2] mas/yr |
Parallax (π) | −0.3793 ± 0.1513 mas[2] |
Distance | 5,500[5] pc |
Details | |
Mass | 0.6[6] M☉ |
Luminosity | 6,550[5] L☉ |
Surface gravity (log g) | 0.5[7] cgs |
Temperature | 6,250[6] K |
Other designations | |
Database references | |
SIMBAD | data |
The visual apparent magnitude of V CrA has been observed to vary between magnitudes 9.4 and 17.9. A maximum magnitude of 8.3 has been estimated from photographic plates.[11] It has around 60% the mass of the Sun and an effective (surface) temperature of around 6250 K.[6]
The spectral class of R0 is typical of a carbon star, but the RCB stars are considered to a separate class of hydrogen-deficient stars, not normal asymptotic giant branch giants.[12]