Astronomy:3 Persei
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Perseus |
| Right ascension | 01h 58m 33.50596s[1] |
| Declination | +49° 12′ 15.6705″[1] |
| Apparent magnitude (V) | 5.70[2] |
| Characteristics | |
| Spectral type | K0 IV[3] |
| Astrometry | |
| Radial velocity (Rv) | −0.67±0.17[4] km/s |
| Proper motion (μ) | RA: +7.051[1] mas/yr Dec.: +41.686[1] mas/yr |
| Parallax (π) | 12.6940 ± 0.0671[1] mas |
| Distance | 257 ± 1 ly (78.8 ± 0.4 pc) |
| Absolute magnitude (MV) | 1.33[2] |
| Details[5] | |
| Mass | 1.41±0.17 M☉ |
| Radius | 8.27±0.55 R☉ |
| Luminosity | 37.2+7.5 −6.3 L☉ |
| Surface gravity (log g) | 2.72±0.09 cgs |
| Temperature | 4,757±25 K |
| Metallicity [Fe/H] | −0.15±0.05 dex |
| Rotational velocity (v sin i) | 1.85±0.45 km/s |
| Age | 2.91±0.98 Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
3 Persei is a single,[7] orange-hued star in the northern constellation of Perseus. It is dimly visible to the naked eye under good viewing conditions, having an apparent visual magnitude of 5.70[2] The star is located around 79 parsecs (257 ly) distant, based upon an annual parallax shift of 12.7 mas.
This star has a stellar classification of K0 IV,[3] suggesting it is a K-type subgiant – an evolved star that has used up its core hydrogen and is evolving to become a red giant. However, da Silva et al. (2015) categorized it as a giant star proper.[8] At the age of around three billion years, it has an estimated 1.4 times the mass of the Sun and has expanded to move than 8 times the Sun's radius. It is radiating roughly 37 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,757 K.[5]
References
- ↑ 1.0 1.1 1.2 1.3 1.4 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940 Gaia DR3 record for this source at VizieR.
- ↑ 2.0 2.1 2.2 Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters 38 (5): 331, doi:10.1134/S1063773712050015, Bibcode: 2012AstL...38..331A.
- ↑ 3.0 3.1 Cowley, A. P.; Bidelman, W. P. (February 1979), "MK spectral types for some F and G stars", Publications of the Astronomical Society of the Pacific 91: 83–86, doi:10.1086/130446, Bibcode: 1979PASP...91...83C
- ↑ de Bruijne, J. H. J.; Eilers, A.-C. (October 2012), "Radial velocities for the HIPPARCOS-Gaia Hundred-Thousand-Proper-Motion project", Astronomy & Astrophysics 546: 14, doi:10.1051/0004-6361/201219219, A61, Bibcode: 2012A&A...546A..61D.
- ↑ 5.0 5.1 Jofré, E. et al. (February 2015), "Stellar parameters and chemical abundances of 223 evolved stars with and without planets", Astronomy & Astrophysics 574: 46, doi:10.1051/0004-6361/201424474, A50, Bibcode: 2015A&A...574A..50J.
- ↑ "3 Per". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=3+Per.
- ↑ Eggleton, P. P.; Tokovinin, A. A. (September 2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society 389 (2): 869–879, doi:10.1111/j.1365-2966.2008.13596.x, Bibcode: 2008MNRAS.389..869E.
- ↑ Da Silva, Ronaldo et al. (2015), "Homogeneous abundance analysis of FGK dwarf, subgiant, and giant stars with and without giant planets", Astronomy & Astrophysics 580: A24, doi:10.1051/0004-6361/201525770, Bibcode: 2015A&A...580A..24D.
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