Astronomy:57 Persei
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Perseus |
| Right ascension | 04h 33m 24.90304s[1] |
| Declination | +43° 03′ 50.0154″[1] |
| Apparent magnitude (V) | 6.078[2] |
| Characteristics | |
| Spectral type | F0 V[3] |
| U−B color index | +0.01[4] |
| B−V color index | +0.38[4] |
| Astrometry | |
| Radial velocity (Rv) | −23.0±4.3[5] km/s |
| Proper motion (μ) | RA: +5.370[1] mas/yr Dec.: +5.531[1] mas/yr |
| Parallax (π) | 16.3759 ± 0.0181[1] mas |
| Distance | 199.2 ± 0.2 ly (61.07 ± 0.07 pc) |
| Absolute magnitude (MV) | +2.23[6] |
| Details | |
| Mass | 1.28[7] M☉ |
| Radius | 2.6[1] R☉ |
| Luminosity | 11.0[1] L☉ |
| Surface gravity (log g) | 3.87[7] cgs |
| Temperature | 6,615±225[7] K |
| Metallicity [Fe/H] | −0.19[8] dex |
| Rotational velocity (v sin i) | 90[3] km/s |
| Age | 1.614[7] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
57 Persei, or m Persei, is a suspected triple star[10] system in the northern constellation of Perseus. It is at the lower limit of visibility to the naked eye, having a combined apparent visual magnitude of 6.08.[2] The annual parallax shift of 16.4 mas provides a distance measure of 199 light years. 57 Persei is moving closer to the Sun with a radial velocity of about −23[5] km/s and will make perihelion in around 2.6 million years at a distance of roughly 22 ly (6.6 pc).[11]
The primary member, 57 Persei, is a magnitude 6.18,[10] yellow-white hued F-type main-sequence star with a stellar classification of F0 V,[3] indicating it is generating energy by fusing its core hydrogen. It is an estimated 1.6[7] billion years old and is spinning with a projected rotational velocity of 90 km/s.[3] The star has 1.3[7] times the mass of the Sun and is radiating 11 times the Sun's luminosity from its photosphere at an effective temperature of around 6,615 K.[7]
An unseen companion has been identified via slight changes to the proper motion of the primary.[10] The third possible member of the system, designated component B,[12] is a magnitude 6.87 F-type star at an angular separation of 120.13 arc seconds.[10] This star has a different parallax and space velocity than the primary,[13] so it may just be a wide visual companion.[12] There are three other nearby visual companions that are not physically associated with the 57 Persei system.[12]
References
- ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 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 Høg, E. et al. (2000), "The Tycho-2 catalogue of the 2.5 million brightest stars", Astronomy and Astrophysics 355: L27, doi:10.1888/0333750888/2862, Bibcode: 2000A&A...355L..27H.
- ↑ 3.0 3.1 3.2 3.3 Royer, F. et al. (February 2007), "Rotational velocities of A-type stars. III. Velocity distributions", Astronomy and Astrophysics 463 (2): 671–682, doi:10.1051/0004-6361:20065224, Bibcode: 2007A&A...463..671R.
- ↑ 4.0 4.1 Dorrit Hoffleit (1991). Combined\bsc5: The Bright Star Catalogue. 5th Ed., Preliminary Version. Yale University Observatory. https://books.google.com/books?id=anECkAEACAAJ.
- ↑ 5.0 5.1 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.
- ↑ Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters 38 (5): 331, doi:10.1134/S1063773712050015, Bibcode: 2012AstL...38..331A.
- ↑ 7.0 7.1 7.2 7.3 7.4 7.5 7.6 David, Trevor J.; Hillenbrand, Lynne A. (2015), "The Ages of Early-Type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets", The Astrophysical Journal 804 (2): 146, doi:10.1088/0004-637X/804/2/146, Bibcode: 2015ApJ...804..146D.
- ↑ Casagrande, L. et al. (June 2011), "New constraints on the chemical evolution of the solar neighbourhood and Galactic disc(s). Improved astrophysical parameters for the Geneva-Copenhagen Survey", Astronomy and Astrophysics 530: A138, doi:10.1051/0004-6361/201016276, Bibcode: 2011A&A...530A.138C.
- ↑ "57 Per". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=57+Per.
- ↑ 10.0 10.1 10.2 10.3 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.
- ↑ Bailer-Jones, C. A. L. (March 2015), "Close encounters of the stellar kind", Astronomy & Astrophysics 575: 13, doi:10.1051/0004-6361/201425221, A35, Bibcode: 2015A&A...575A..35B.
- ↑ 12.0 12.1 12.2 Mason, B. D. et al. (2014), "The Washington Visual Double Star Catalog", The Astronomical Journal 122 (6): 3466, doi:10.1086/323920, Bibcode: 2001AJ....122.3466M
- ↑ 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.
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