3 Persei
| Observation data Epoch J2000 Equinox ICRS | |
|---|---|
| Constellation | Perseus |
| Right ascension | 01h 58m 33.50596s[1] |
| Declination | +49° 12′ 15.6705″[1] |
| Apparent magnitude (V) | 5.70[2] |
| Characteristics | |
| Evolutionary stage | red giant branch[1] |
| 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 mas[1] |
| 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 | |
| 3 Per, BD+48°576, HD 11949, HIP 9222, HR 568, SAO 37665[6] | |
| 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
[edit]- 1 2 3 4 5 6 Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
- 1 2 3 Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv:1108.4971, Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015, S2CID 119257644.
- 1 2 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, Bibcode:1979PASP...91...83C, doi:10.1086/130446
- ↑ 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, arXiv:1208.3048, Bibcode:2012A&A...546A..61D, doi:10.1051/0004-6361/201219219, S2CID 59451347, A61.
- 1 2 Jofré, E.; et al. (February 2015), "Stellar parameters and chemical abundances of 223 evolved stars with and without planets", Astronomy & Astrophysics, 574: 46, arXiv:1410.6422, Bibcode:2015A&A...574A..50J, doi:10.1051/0004-6361/201424474, S2CID 53666931, A50.
- ↑ "3 Per". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-03-08.
- ↑ 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, arXiv:0806.2878, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x, S2CID 14878976.
- ↑ 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, arXiv:1505.01726, Bibcode:2015A&A...580A..24D, doi:10.1051/0004-6361/201525770, S2CID 119216425.
