57 Tauri

57 Tauri

A light curve for V483 Tauri, plotted from TESS data.[1]
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]
Distance148.4 ± 0.4 ly
(45.5 ± 0.1 pc)
Absolute magnitude (MV)5.56[6]
Orbit[7]
Primaryδ 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
Mass1.6[2] M☉
Radius2.0[2] R☉
Luminosity9.8[2] L☉
Surface gravity (log g)4.00[2] cgs
Temperature7,258[2] K
Metallicity [Fe/H]0.051[8] dex
Rotation0.905 d[9]
Rotational velocity (v sin i)97.6[9] km/s
Age1.2[2] Gyr
Other designations
h Tauri, HD 27397, V0483 Tauri, HR 1351, HIP 20219, SAO 93872, BD+13 663[10]
Database references
SIMBADdata

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]

  1. ^ Cite error: The named reference MAST was invoked but never defined (see the help page).
  2. ^ a b c d e f g h i j k l Cite error: The named reference dr3 was invoked but never defined (see the help page).
  3. ^ a b c d Cite error: The named reference gcvs was invoked but never defined (see the help page).
  4. ^ Cite error: The named reference Gray2001 was invoked but never defined (see the help page).
  5. ^ Cite error: The named reference Böhm-Vitense2002 was invoked but never defined (see the help page).
  6. ^ Cite error: The named reference cesetti2013 was invoked but never defined (see the help page).
  7. ^ a b Cite error: The named reference Kaye1999 was invoked but never defined (see the help page).
  8. ^ Cite error: The named reference huber2016 was invoked but never defined (see the help page).
  9. ^ a b Cite error: The named reference vs2013 was invoked but never defined (see the help page).
  10. ^ Cite error: The named reference SIMBAD was invoked but never defined (see the help page).
  11. ^ a b Cite error: The named reference Paparó2000 was invoked but never defined (see the help page).
  12. ^ Cite error: The named reference Boss1908 was invoked but never defined (see the help page).
  13. ^ Cite error: The named reference vanBueren1952 was invoked but never defined (see the help page).
  14. ^ Cite error: The named reference Freund2020 was invoked but never defined (see the help page).
  15. ^ Cite error: The named reference Millis1967 was invoked but never defined (see the help page).
  16. ^ Cite error: The named reference Kukarkin1972 was invoked but never defined (see the help page).