50 Persei
Star in the constellation Perseus
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50 Persei is a star in the constellation Perseus. Its apparent magnitude is 5.52,[2] which is bright enough to be seen with the naked eye. Located around 21.00 parsecs (68.5 ly) distant, it is a White main-sequence star of spectral type F7V,[4] a star that is currently fusing its core hydrogen. In 1998 the star was named a candidate Gamma Doradus variable with a period of 3.05 days,[6] which would means it displays variations in luminosity due to non-radial pulsations in the photosphere. Subsequently, it was classified as a RS Canum Venaticorum and BY Draconis variable by an automated program.[13]
  | |
| Observation data Epoch J2000.0 Equinox ICRS | |
|---|---|
| Constellation | Perseus |
| Right ascension | 04h 08m 36.61660s[1] |
| Declination | +38° 02′ 23.0488″[1] |
| Apparent magnitude (V) | 5.52[2] |
| Characteristics | |
| Evolutionary stage | main sequence[3] |
| Spectral type | F7 V[4] |
| U−B color index | +0.00[2] |
| B−V color index | +0.54[2] |
| Variable type | RS CVn and BY Dra |
| Astrometry | |
| Radial velocity (Rv) | +26.2[5] km/s |
| Proper motion (μ) | RA: +164.10[1] mas/yr Dec.: −202.60[1] mas/yr |
| Parallax (π) | 47.63±0.26 mas[1] |
| Distance | 68.5 ± 0.4 ly (21.0 ± 0.1 pc) |
| Absolute magnitude (MV) | 3.87[6] |
| Details | |
| Mass | 1.30[7] M☉ |
| Radius | 1.22[7] R☉ |
| Luminosity | 2.3[7] L☉ |
| Surface gravity (log g) | 4.38[7] cgs |
| Temperature | 6,429[7] K |
| Metallicity [Fe/H] | −0.11[8] dex |
| Rotation | 2.71 days[9] |
| Rotational velocity (v sin i) | 20.81[10] km/s |
| Age | 600[11] Myr |
| Other designations | |
| 50 Per, BD+37°882, FK5 2297, GJ 9145, HD 25998, HIP 19335, V582 Persei, HR 1278, SAO 57006.[12] | |
| Database references | |
| SIMBAD | data |
This is probably a binary system with an unseen companion. It is physically associated with the likely binary system HIP 19255, with the two pairs orbiting each other over a time scale of around a million years. The components of HIP 19255 have an angular separation of 3.87″ and the two components orbit each other every 590 years. 50 Persei may share a gravitational association with Capella, even though the two are separated by nearly 15° − equivalent to a distance of 19 ly (5.9 pc).[15]
50 Persei is emitting an infrared excess at a wavelength of 70 μm, suggesting the presence of a circumstellar debris disk. The disk has a temperature of 96±5 K.[11]