HD 28527
HD 28527 is a star in the constellation Taurus, and a member of the Hyades open cluster. It is faintly visible to the naked eye with an apparent visual magnitude of 4.78. The distance to this star, as determined from its parallax shift of 22 mas, is 148 light years. It is moving away from the Earth with a heliocentric radial velocity of +38 km/s.
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Taurus |
| Right ascension | 04h 30m 33.633s |
| Declination | +16° 11′ 38.46″ |
| Apparent magnitude (V) | 4.78 |
| Characteristics | |
| Spectral type | A6 IV or A7 V |
| B−V color index | +0.170±0.001 |
| Variable type | suspected δ Sct |
| Astrometry | |
| Radial velocity (Rv) | +38.1±0.8 km/s |
| Proper motion (μ) | RA: +104.422 mas/yr Dec.: −26.254 mas/yr |
| Parallax (π) | 22.0357 ± 0.2516 mas |
| Distance | 148 ± 2 ly (45.4 ± 0.5 pc) |
| Absolute magnitude (MV) | +1.58 |
| Details | |
| Mass | 1.75 M☉ |
| Radius | 2.209 R☉ |
| Luminosity | 19.03 L☉ |
| Surface gravity (log g) | 4.17±0.14 cgs |
| Temperature | 8,274±281 K |
| Metallicity [Fe/H] | +0.30 dex |
| Rotation | 1.278 d |
| Rotational velocity (v sin i) | 87.5 km/s |
| Age | 307 Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
Based upon a stellar classification of A6 IV by Cowley et al. (1969), 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. At the age of 307 million years, it has a high rate of spin, revolving upon its axis once every 1.278 days. It is a Delta Scuti variable with 1.75 times the mass of the Sun and 2.2 times the Sun's radius. The star is radiating 19 times the Sun's luminosity from its photosphere at an effective temperature of 8,274 K.
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. 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″.