Gamma Volantis
Gamma Volantis, Latinized from γ Volantis, is a wide binary star system in the southern constellation of Volans. Based upon parallax measurements, it is approximately 133 light years from Earth. It is bright enough to be seen with the naked eye and can be found around 9° to the east-southeast of the Large Magellanic Cloud.
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Volans |
| γ1 Vol | |
| Right ascension | 07h 08m 42.3703s |
| Declination | −70° 29′ 49.527″ |
| Apparent magnitude (V) | 5.704 |
| γ2 Vol | |
| Right ascension | 07h 08m 44.8657s |
| Declination | −70° 29′ 56.149″ |
| Apparent magnitude (V) | 3.62 |
| Characteristics | |
| Spectral type | F2V + K0III |
| Astrometry | |
| γ1 Vol | |
| Radial velocity (Rv) | −3 km/s |
| Proper motion (μ) | RA: 11.069(437) mas/yr Dec.: 107.302(577) mas/yr |
| Parallax (π) | 22.7501 ± 0.4619 mas |
| Distance | 143 ± 3 ly (44.0 ± 0.9 pc) |
| Absolute magnitude (MV) | 2.51 |
| γ2 Vol | |
| Radial velocity (Rv) | +2.8 km/s |
| Proper motion (μ) | RA: 23.620(154) mas/yr Dec.: 108.653(170) mas/yr |
| Parallax (π) | 24.4775 ± 0.1130 mas |
| Distance | 133.2 ± 0.6 ly (40.9 ± 0.2 pc) |
| Details | |
| γ1 Vol | |
| Mass | 1.69 M☉ |
| Surface gravity (log g) | 2.71 cgs |
| Temperature | 6,541 K |
| Metallicity [Fe/H] | +0.12 dex |
| Rotational velocity (v sin i) | 4.4±0.2 km/s |
| Age | 1.4 Gyr |
| γ2 Vol | |
| Luminosity | 60 L☉ |
| Surface gravity (log g) | 2.7±0.1 cgs |
| Temperature | 4,866±34 K |
| Metallicity [Fe/H] | −0.01±0.03 dex |
| Other designations | |
| γ1 Vol: HD 55864, HIP 34473, HR 2735, SAO 256373 | |
| γ2 Vol: HD 55865, HIP 34481, HR 2736, SAO 256374 | |
| Database references | |
| SIMBAD | γ1 Vol |
| γ2 Vol | |
The brighter component, designated γ2 Volantis, is an orange K-type giant star with a stellar classification of K0 III and an apparent magnitude of +3.62, making this the brightest star in the constellation. Its companion, γ1 Volantis, is an F-type main-sequence star of classification F2 V and an apparent magnitude of +5.70. As of 2002, the pair were at an angular separation of 14.1″ along a position angle of 296°. Their separation has decreased from 15.7″ in 1826. The secondary is a source of X-ray emission with a luminosity of 8.3×1028 erg s−1.