| |
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Taurus |
| Right ascension | 04h19m 57.70457s[2] |
| Declination | +14° 02′ 06.7322″[2] |
| Apparent magnitude (V) | 5.55 - 5.59[3] |
| Characteristics | |
| Spectral type | F0 IV[4] |
| B−V color index | 0.283[5] |
| Variable type | δ Scuti[3] |
| Astrometry | |
| Proper motion (μ) | RA: 115.369±0.078[2] mas/yr Dec.: −18.825±0.052[2] mas/yr |
| Parallax (π) | 21.9777 ± 0.0621 mas[2] |
| Distance | 148.4 ± 0.4 ly (45.5 ± 0.1 pc) |
| Absolute magnitude (MV) | 5.56[6] |
| Orbit[7] | |
| Primary | δ Scuti star |
| Period (P) | 2.4860±0.0017 d |
| Eccentricity (e) | 0.028±0.010 |
| Longitude of the node (Ω) | 140.5±20.4° |
| Periastron epoch (T) | 2451164.968±0.144 |
| Semi-amplitude (K1) (primary) | 29.906±0.316 km/s |
| Details | |
| Mass | 1.6[2] M☉ |
| Radius | 2.0[2] R☉ |
| Luminosity | 9.8[2] L☉ |
| Surface gravity (log g) | 4.00[2] cgs |
| Temperature | 7,258[2] K |
| Metallicity [Fe/H] | 0.051[8] dex |
| Rotation | 0.905 d[9] |
| Rotational velocity (v sin i) | 97.6[9] km/s |
| Age | 1.2[2] Gyr |
| Other designations | |
h Tauri, HD 27397, V0483 Tauri, HR 1351, HIP 20219, SAO 93872, BD+13 663[10] | |
| Database references | |
| SIMBAD | data |
57 Tauri, also known as h Tauri and V483 Tauri, is a star 148 light years from the Earth, in the constellation Taurus.[2] It is a 5th magnitude star, so it will be visible to the naked eye of an observer located far from city lights.[3] 57 Tauri is a member of the Hyades star cluster.[11] It is a Delta Scuti variable star, whose brightness changes slightly, ranging from magnitude 5.55 to 5.59.[3]
In 1908, Lewis Boss listed 57 Tauri as a member of the Hyades cluster based upon its proper motion agreeing with the motions of other cluster members.[12] Its membership in the cluster was firmly established forty-four years later by Hendrik van Bueren, using both proper motion and radial velocity.[13] 57 Tauri is located 10.8 light years from the core of the Hyades cluster.[14]
Robert Millis discovered that 57 Tauri is a variable star, in 1967. He reported that the amplitude varied by 0.02 magnitudes with a period of 1.5 hours.[15] In 1972, it was given the variable star designation V483 Tauri.[16] A year 2000 study of 57 Tauri, based on 54 nights of photometric data, identified twelve pulsation frequencies ranging in period from 58.6 minutes to 6.17 days.[11]
In 1999, Anthony Kaye discovered that 57 Tauri is a spectroscopic binary by examining 139 high signal-to-noise spectra obtained at Kitt Peak.[7]
