132 Tauri
132 Tauri is a binary star system in the constellation Taurus. It is faintly visible to the naked eye with an apparent visual magnitude of 4.89. Based upon a poorly-constrained annual parallax shift of 8.97±1.98 mas, it is located roughly 360 light years from the Sun. The system is moving further away with a heliocentric radial velocity of +16 km/s. It lies near the ecliptic and thus is subject to occultation by the Moon. One such event was observed September 3, 1991.
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Taurus |
| Right ascension | 05h 49m 00.96598s |
| Declination | +24° 34′ 03.1220″ |
| Apparent magnitude (V) | 4.89 (5.07 + 9.09) |
| Characteristics | |
| Spectral type | G9 III |
| B−V color index | 1.021 |
| Astrometry | |
| Radial velocity (Rv) | +15.8±0.6 km/s |
| Proper motion (μ) | RA: +10.44 mas/yr Dec.: −8.30 mas/yr |
| Parallax (π) | 8.97 ± 1.98 mas |
| Distance | approx. 360 ly (approx. 110 pc) |
| Details | |
| 132 Tau Aa | |
| Surface gravity (log g) | 2.74±0.11 cgs |
| Temperature | 4,853±47 K |
| Metallicity [Fe/H] | 0.18±0.05 dex |
| Other designations | |
| Database references | |
| SIMBAD | data |
This system forms a wide double star with an angular separation of 3.8″ along a position angle of 230°, as of 1991. The brighter star, component A, has an apparent magnitude of 4.99 while the fainter secondary, component B, is of magnitude 9.09. The primary is itself an unresolved binary with a combined stellar classification of G9 III, which matches an aging G-type giant star that has exhausted the hydrogen at its core and evolved away from the main sequence.