Observation data Epoch J2000.0 Equinox J2000.0 | |
---|---|
Constellation | Taurus |
Right ascension | 04h 19m 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 | |
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]
Observation data Epoch J2000.0 Equinox J2000.0 | |
---|---|
Constellation | Taurus |
Right ascension | 04h 19m 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 | |
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]