HD 28527

HD 28527
Observation data
Epoch J2000      Equinox J2000
Constellation Taurus
Right ascension 04h 30m 33.633s[1]
Declination +16° 11′ 38.46″[1]
Apparent magnitude (V) 4.78[2]
Characteristics
Spectral type A6 IV[3] or A7 V[4]
B−V color index +0.170±0.001[2]
Variable type suspected δ Sct[5]
Astrometry
Radial velocity (Rv)+38.1±0.8[2] km/s
Proper motion (μ) RA: +104.422[1] mas/yr
Dec.: −26.254[1] mas/yr
Parallax (π)22.0357 ± 0.2516 mas[1]
Distance148 ± 2 ly
(45.4 ± 0.5 pc)
Absolute magnitude (MV)+1.58[6]
Details
Mass1.75[7] M☉
Radius2.209[8] R☉
Luminosity19.03[2] L☉
Surface gravity (log g)4.17±0.14[7] cgs
Temperature8,274±281[7] K
Metallicity [Fe/H]+0.30[9] dex
Rotation1.278 d[8]
Rotational velocity (v sin i)87.5[8] km/s
Age307[7] Myr
Other designations
NSV 1627, BD+15°637, GJ 170.1/9157, HD 28527, HIP 21029, HR 1427, SAO 93975[10]
Database references
SIMBADdata
Hyades cluster, with HD 28527 (marked with a green arrow) just NE of the θ Tauri pair

HD 28527 is a star in the constellation Taurus, and a member of the Hyades open cluster.[8] It is faintly visible to the naked eye with an apparent visual magnitude of 4.78.[2] The distance to this star, as determined from its parallax shift of 22 mas,[1] is 148 light years. It is moving away from the Earth with a heliocentric radial velocity of +38 km/s.[2]

Based upon a stellar classification of A6 IV by Cowley et al. (1969),[3] this is an A-type subgiant star that has consumed the hydrogen at its core and is evolving away from the main sequence. Older studies had it classed as an A-type main-sequence star with a class of A7 V.[4] At the age of 307[7] million years, it has a high rate of spin, revolving upon its axis once every 1.278 days.[8] It is a Delta Scuti variable[5] with 1.75[7] times the mass of the Sun and 2.2[8] times the Sun's radius. The star is radiating 19[2] times the Sun's luminosity from its photosphere at an effective temperature of 8,274 K.[7]

Due to its location near the ecliptic, this star is subject to lunar occultations. These events have provided occasional, but not definitive, evidence of a close secondary companion.[11][12] Eggleton and Tokovinin (2008) catalogue this as a possible triple star system, having the inner pair being similar stars with an angular separation of 0.02″, and the outer component a magnitude 6.7 star of class F2 at a much wider separation of 250″.[13]

  1. ^ a b c d e f Cite error: The named reference GaiaDR2 was invoked but never defined (see the help page).
  2. ^ a b c d e f g Cite error: The named reference Anderson2012 was invoked but never defined (see the help page).
  3. ^ a b Cite error: The named reference Cowley1969 was invoked but never defined (see the help page).
  4. ^ a b Cite error: The named reference Ljunggren1961 was invoked but never defined (see the help page).
  5. ^ a b Cite error: The named reference gcvs was invoked but never defined (see the help page).
  6. ^ Cite error: The named reference Eggen1998 was invoked but never defined (see the help page).
  7. ^ a b c d e f g Cite error: The named reference David2015 was invoked but never defined (see the help page).
  8. ^ a b c d e f Cite error: The named reference vanSaders2013 was invoked but never defined (see the help page).
  9. ^ Cite error: The named reference Gebran2010 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. ^ Cite error: The named reference Peterson1981 was invoked but never defined (see the help page).
  12. ^ Cite error: The named reference Richichi1999 was invoked but never defined (see the help page).
  13. ^ Cite error: The named reference Eggleton2008 was invoked but never defined (see the help page).