| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Taurus |
| Right ascension | 04h30m 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] |
| Distance | 148 ± 2 ly (45.4 ± 0.5 pc) |
| Absolute magnitude (MV) | +1.58[6] |
| Details | |
| Mass | 1.75[7] M☉ |
| Radius | 2.209[8] R☉ |
| Luminosity | 19.03[2] L☉ |
| Surface gravity (log g) | 4.17±0.14[7] cgs |
| Temperature | 8,274±281[7] K |
| Metallicity [Fe/H] | +0.30[9] dex |
| Rotation | 1.278 d[8] |
| Rotational velocity (v sin i) | 87.5[8] km/s |
| Age | 307[7] Myr |
| Other designations | |
NSV 1627, BD+15°637, GJ 170.1/9157, HD 28527, HIP 21029, HR 1427, SAO 93975[10] | |
| Database references | |
| SIMBAD | data |
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 shiftof22 mas,[1]is148 light years. It is moving away from the Earth with a heliocentric radial velocityof+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 separationof0.02″, and the outer component a magnitude 6.7 star of class F2 at a much wider separation of 250″.[13]
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