Observation data Epoch J2000.0 Equinox J2000.0 | |
---|---|
Constellation | Corvus |
Right ascension | 12h 37m 40.711s[2] |
Declination | −19° 34′ 40.03″[2] |
Apparent magnitude (V) | 8.77[3] (8.6 - 9.16)[4] |
Characteristics | |
Evolutionary stage | Main sequence |
Spectral type | F0V[5] (F0 + G0)[6] |
B−V color index | 0.404±0.026[3] |
Variable type | β Lyr[7] |
Astrometry | |
Radial velocity (Rv) | 19.0±4.6[8] km/s |
Proper motion (μ) | RA: −29.326 mas/yr[2] Dec.: 8.954 mas/yr[2] |
Parallax (π) | 4.7351 ± 0.0812 mas[2] |
Distance | 690 ± 10 ly (211 ± 4 pc) |
Absolute magnitude (MV) | 2.32[3] |
Orbit[9] | |
Period (P) | 0.7473 d |
Eccentricity (e) | 0.00 |
Periastron epoch (T) | 2445792.3578 |
Argument of periastron (ω) (secondary) | 0.00° |
Semi-amplitude (K1) (primary) | 64 km/s |
Semi-amplitude (K2) (secondary) | 235 km/s |
Details | |
Primary | |
Mass | 1.64±0.14[9] M☉ |
Radius | 2.16 or 2.18 ± 0.08[9] R☉ |
Luminosity | 8.4 or 8.5 ± 0.6[9] L☉ |
Secondary | |
Mass | 0.44±0.03[9] M☉ |
Radius | 1.19 or 1.20 ±0.04[9] R☉ |
Luminosity | 1.2 or 1.5 ± 0.1[9] L☉ |
Other designations | |
Database references | |
SIMBAD | data |
RV Corvi is an eclipsing binary star system in the southern constellation of Corvus. The brightness of the pair regularly ranges in apparent visual magnitude from 8.6 down to 9.16 over a period 18 hours,[4] even the brightest of which is too faint to be visible to the naked eye. The system is located at a distance of approximately 690 light-years from the Sun based on parallax measurements, and is drifting further away with a radial velocity of ~19 km/s.[8]
The variability of this system was discovered by H. H. Swope.[11] In 1942, Irene G. Buttery published an orbital period of 0.74728 days for the system, showing this is an eclipsing binary.[12] It is a near-contact binary with both stars showing the effect of tidal interactions and the facing sides are less than 10% of the orbital separation apart, but are not in contact.[13] One or both stars may show an excess of luminosity on their facing sides.[9] The system is composed of stars of spectral types F0 and G0, which orbit each other every 0.7473 days.[6]
MAST
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