S Persei
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  | |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Perseus |
| Right ascension | 2h 22m 51.70928s[1] |
| Declination | 58° 31′ 11.4476″[1] |
| Apparent magnitude (V) | 9.23[2] (7.9 - 12.0[3]) |
| Characteristics | |
| Spectral type | M4.5I[2] (M3Iae - M7[3]) |
| B−V color index | 2.65[2] |
| Variable type | SRc[3] |
| Astrometry | |
| Radial velocity (Rv) | -39.71[4] km/s |
| Proper motion (μ) | RA: −0.49 ± 0.23[5] mas/yr Dec.: −1.19 ± 0.20[5] mas/yr |
| Parallax (π) | 0.413 ± 0.017[5] mas |
| Distance | 7,900 ± 300 ly (2,420 ± 100 pc) |
| Absolute magnitude (MV) | −6.36 (at mV 9.23)[2] |
| Details | |
| Mass | 20[6] M☉ |
| Radius | 1,212 ± 124[7], 780 - 1,230[2] R☉ |
| Luminosity | 86,000 - 186,000[8][9][10] L☉ |
| Surface gravity (log g) | 0.0[11] cgs |
| Temperature | 3,000[12]–3,600[8] K |
| Other designations | |
| Database references | |
| SIMBAD | data |
S Persei is a red supergiant located within the Double Cluster in the Perseus constellation. The star was discovered by File:Flag of de.svg German astronomer Adalbert Krueger in 1874 after observing that it varied in brightness, and thus, luminosity.
Properties[edit]
S Persei is a red hypergiant[13] with a stellar classification estimated to be between M3 to M8,[14] which gives the star a temperature of 3,000 to 3,600 degrees Kelvin.[15] S Persei has a mass of 20 M☉[16] and a luminosity of 86,000 - 186,000 L☉.[17] However, S Persei's angular diameter has been measured and found to be somewhat elliptical; modelled as a uniform disk, the radius results to 1,212 ± 124 R☉.[18]
Size[edit]
S Persei's radius is estimated to be 780 R☉, but could be as large as 1,230 R☉.[19]
References[edit]
- ↑ 1.0 1.1 Cite error: Invalid
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<ref>tag; no text was provided for refs namedthompson - ↑ 8.0 8.1 Cite error: Invalid
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<ref>tag; no text was provided for refs namedgonzalez - ↑ Cite error: Invalid
<ref>tag; no text was provided for refs namedGarciaHernandez - ↑ https://doi.org/10.1051/0004-6361/201219587
- ↑ http://adsabs.harvard.edu/abs/2009ASPC..412..113W
- ↑ https://doi.org/10.1051/0004-6361%3A20065785
- ↑ https://doi.org/10.1093/mnras/270.4.958
- ↑ https://doi.org/10.1051/0004-6361/20079063
- ↑ http://adsabs.harvard.edu/abs/2003AAS...203.4907T
- ↑ https://doi.org/10.1086/430901
