132 Tauri is a binary star[2] system in the constellation Taurus. It is faintly visible to the naked eye with an apparent visual magnitude of 4.89.[2] Based upon a poorly-constrained annual parallax shift of 8.97±1.98 mas,[1] 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.[5] It lies near the ecliptic and thus is subject to occultation by the Moon. One such event was observed September 3, 1991.[8]
Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Taurus |
Right ascension | 05h 49m 00.96598s[1] |
Declination | +24° 34′ 03.1220″[1] |
Apparent magnitude (V) | 4.89 (5.07 + 9.09)[2] |
Characteristics | |
Spectral type | G9 III[3] |
B−V color index | 1.021[4] |
Astrometry | |
Radial velocity (Rv) | +15.8±0.6[5] km/s |
Proper motion (μ) | RA: +10.44[1] mas/yr Dec.: −8.30[1] mas/yr |
Parallax (π) | 8.97 ± 1.98 mas[1] |
Distance | approx. 360 ly (approx. 110 pc) |
Details | |
132 Tau Aa | |
Surface gravity (log g) | 2.74±0.11[6] cgs |
Temperature | 4,853±47[6] K |
Metallicity [Fe/H] | 0.18±0.05[6] 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[9] with a combined stellar classification of G9 III,[3] which matches an aging G-type giant star that has exhausted the hydrogen at its core and evolved away from the main sequence.