RS Persei
| Observation data Epoch J2000 Equinox J2000 |
|
|---|---|
| Constellation | Perseus |
| Right ascension | 2h 22m 24.297s[1] |
| Declination | +57° 0.6′ 34.36″[1] |
| Apparent magnitude (V) | 7.82-10.0[2] |
| Characteristics | |
| Spectral type | M4Iab[3] |
| Variable type | SRc[2] |
| Astrometry | |
| Radial velocity (Rv) | -38.0±2[4] km/s |
| Proper motion (μ) | RA: -5.7±1.8[5] mas/yr Dec.: -1.4±1.7[5] mas/yr |
| Distance | 2,345±55[6] pc |
| Absolute magnitude (MV) | −6.18[7] |
| Details[6] | |
| Mass | 12-15 M☉ |
| Radius | 740-800 R☉ |
| Luminosity | 70,000 - 87,000 L☉ |
| Surface gravity (log g) | −0.2 ± 0.05 cgs |
| Temperature | 3470 ± 90 K |
| Other designations | |
| Database references | |
| SIMBAD | data |
RS Persei is a red supergiant variable star located in the Double Cluster in Perseus. Its brightness varies from magnitude 7.82 to 10.0.
Location
RS Persei is a member of the cluster NGC 884, χ Persei, one half of the famous Double Cluster.[8]
Variability
RS Persei is classified as a semiregular variable star, with its brightness varying from magnitude 7.82 to 10.0 over 245 days,[2] Detailed studies show that it also pulsates with a long secondary period period of 4200 ± 1500 days.[9]
Properties
RS Persei is a large cool star, 3,500 K and over 700 R☉. This makes it luminous, although much of its radiation is emitted in the infrared. Across all wavelengths it is at least 70,000 times as luminous as the sun. It is surrounded by dust that has condensed from material lost by the star.[10]
RS Persei has sometimes been considered to be a highly evolved low mass Asymptotic Giant Branch (AGB) star,[11] but calculations of its current mass suggest that it is a low mass supergiant. NGC 244 is also too young to host AGB stars.[6]
References
- ↑ 1.0 1.1 Lua error in package.lua at line 80: module 'strict' not found.
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