Delta Persei
 Location of δ Persei (circled) |
|
| Observation data Epoch J2000 Equinox J2000 |
|
|---|---|
| Constellation | Perseus |
| Right ascension | 03h 42m 55.50426s |
| Declination | +47° 47′ 15.1746″ |
| Apparent magnitude (V) | 3.01 |
| Characteristics | |
| Spectral type | B5 III |
| U−B color index | –0.51 |
| B−V color index | –0.12 |
| Astrometry | |
| Radial velocity (Rv) | +4 km/s |
| Proper motion (μ) |
RA: +25.58 mas/yr Dec.: −43.06 mas/yr |
| Parallax (π) | 6.32 ± 0.47mas |
| Distance | 520 ± 40 ly (160 ± 10 pc) |
| Details | |
| Mass | 7.0 ± 0.3 M☉ |
| Radius | 10.5 R☉ |
| Surface gravity (log g) | 3.5 cgs |
| Temperature | 14,890 K |
| Rotational velocity (v sin i) | 190 km/s |
| Age | 50.1 ± 6.8 Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
Delta Persei (Delta Per, δ Persei, δ Per) is a double star in the northern constellation of Perseus. It has an apparent visual magnitude of 3.01, making it readily visible with the naked eye. Parallax measurements give it a distance of about 520 light-years (160 parsecs) from the Earth.
The spectrum of this star matches a stellar classification of B5 III, which indicates it is a giant star that has evolved away from the main sequence after exhausting the hydrogen at its core. It has about seven times the Sun's mass and has an estimated age of 6.8 million years. The effective temperature of the outer envelope is 14,890 K, with the energy being emitted at this temperature giving it the blue-white hue that is a characteristic of a B-type star. It is rotating rapidly with a projected rotational velocity of 190 km s−1, which gives a lower bound for the actual azimuthal velocity along the star's equator.
This is most probably a binary star and may be a triple star system. It has an optical companion with an apparent magnitude of +6.17 at an angular separation of 0.330 arcseconds and a position angle of 221°, but it is uncertain whether this is an optical double star or a gravitationally bound companion. The star has also been categorized as a spectroscopic binary, indicating that it has an orbiting companion that has not been separately resolved with a telescope. Finally, this star may be a member of the Melotte 20 open cluster, which would make it the second-brightest member after Mirfak.
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