Observation data Epoch J2000.0 Equinox J2000.0 | |
---|---|
Constellation | Perseus |
Right ascension | 04h 08m 36.61660s [2] |
Declination | +38° 02′ 23.0488″ [2] |
Apparent magnitude (V) | 5.52 [3] |
Characteristics | |
Spectral type | F7 V [4] |
U−B color index | +0.00 [3] |
B−V color index | +0.54 [3] |
Variable type | RS CVn and BY Dra |
Astrometry | |
Radial velocity (Rv) | +26.2 [5] km/s |
Proper motion (μ) |
RA: +164.10
[2]
mas/
yr Dec.: −202.60 [2] mas/ yr |
Parallax (π) | 47.63 ± 0.26 mas [2] |
Distance | 68.5 ± 0.4
ly (21.0 ± 0.1 pc) |
Absolute magnitude (MV) | 3.87 [6] |
Details | |
Mass | 1.16 [7] M☉ |
Surface gravity (log g) | 4.35 [7] cgs |
Temperature | 6,147 [7] K |
Metallicity [Fe/H] | −0.11 [7] dex |
Rotational velocity (v sin i) | 20.81 [8] km/s |
Age | 0.60 [9] Gyr |
Other designations | |
Database references | |
SIMBAD | data |
50 Persei is a star in the constellation Perseus. Its apparent magnitude is 5.52, [3] 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. [11]
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). [12]
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. [9]
Observation data Epoch J2000.0 Equinox J2000.0 | |
---|---|
Constellation | Perseus |
Right ascension | 04h 08m 36.61660s [2] |
Declination | +38° 02′ 23.0488″ [2] |
Apparent magnitude (V) | 5.52 [3] |
Characteristics | |
Spectral type | F7 V [4] |
U−B color index | +0.00 [3] |
B−V color index | +0.54 [3] |
Variable type | RS CVn and BY Dra |
Astrometry | |
Radial velocity (Rv) | +26.2 [5] km/s |
Proper motion (μ) |
RA: +164.10
[2]
mas/
yr Dec.: −202.60 [2] mas/ yr |
Parallax (π) | 47.63 ± 0.26 mas [2] |
Distance | 68.5 ± 0.4
ly (21.0 ± 0.1 pc) |
Absolute magnitude (MV) | 3.87 [6] |
Details | |
Mass | 1.16 [7] M☉ |
Surface gravity (log g) | 4.35 [7] cgs |
Temperature | 6,147 [7] K |
Metallicity [Fe/H] | −0.11 [7] dex |
Rotational velocity (v sin i) | 20.81 [8] km/s |
Age | 0.60 [9] Gyr |
Other designations | |
Database references | |
SIMBAD | data |
50 Persei is a star in the constellation Perseus. Its apparent magnitude is 5.52, [3] 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. [11]
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). [12]
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. [9]