Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Virgo |
Right ascension | 13h 02m 37.981s[2] |
Declination | +05° 11′ 08.36″[2] |
Apparent magnitude (V) | 7.7 to 9.7[3] |
Characteristics | |
Evolutionary stage | AGB[4] |
Spectral type | M8III[5] |
B−V color index | 1.352±0.031[6] |
Variable type | SRb[7] |
Astrometry | |
Radial velocity (Rv) | 17.3±0.2[4] km/s |
Proper motion (μ) | RA: +37.037 mas/yr[2] Dec.: −17.714 mas/yr[2] |
Parallax (π) | 4.417 ± 0.134 mas[3] |
Distance | 740 ± 20 ly (226 ± 7 pc) |
Absolute magnitude (MV) | 2.94[6] |
Details | |
Mass | 1.5[8] M☉ |
Radius | 390[9] R☉ |
Luminosity (bolometric) | 5,012+1,154 −938[4] L☉ |
Surface gravity (log g) | +0.21[10] cgs |
Temperature | 2,902[10] K |
Metallicity [Fe/H] | −0.33[10] dex |
Other designations | |
Database references | |
SIMBAD | data |
RT Virginis is a variable star in the equatorial constellation of Virgo, abbreviated RT Vir. It ranges in brightness from an apparent visual magnitude of 7.7 down to 9.7,[3] which is too faint to be visible to the naked eye. Based on parallax measurements made with the VLBI, the distance to this star is approximately 740 light years.[3] It is receding from the Sun with a radial velocity of 17 km/s.[4]
The long period variability of this star was discovered by W. P. Fleming in 1896, based on photographic plates taken between 1886 and 1895.[12] A. H. Joy in 1942 categorized it as an irregular variable with a stellar classification of M8III.[5] In 1969 it was classified as a semiregular variable star of the SRb type.[13] The period was determined to be 155 days by P. N. Kholopov and associates in 1985, then re-evaluated as 375 days based on AAVSO light curves in 1997. This is an oxygen-rich red giant star on the asymptotic giant branch of its evolution, and is undergoing mass loss due to thermal pulsation.[9]
Water vapor emission in the vicinity of the star was detected in the microwave band by D. F. Dickinson in 1973.[14] This is originating from strong maser emission in a circumstellar gas-dust shell.[15] The flux density of these water masers is over 100 Jy.[9] The star is losing mass at a rate of 3×10−6 M☉·yr−1;[8] the equivalent of the Sun's mass in 3.3 million years. The velocity of the spherically expanding gas is as high as 11 km/s in the water maser region, at a radius of 5 to 25 AU. In a SiO emitting region located ~400 AU from the star, the gas velocity is 7.8 km/s.[16] This outflow appears clumpy and asymmetrical[17] with a strong temporal variation.[15]
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