57 Persei
Observation data
Epoch J2000      Equinox J2000
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 mas[1]
Distance199.2 ± 0.2 ly
(61.07 ± 0.07 pc)
Absolute magnitude (MV)+2.23[6]
Details
Mass1.28[7] M☉
Radius2.6[1] R☉
Luminosity11.0[1] L☉
Surface gravity (log g)3.87[7] cgs
Temperature6,615±225[7] K
Metallicity [Fe/H]−0.19[8] dex
Rotational velocity (v sin i)90[3] km/s
Age1.614[7] Gyr
Other designations
m Per, 57 Per, BD+42°990, FK5 1124, HD 28704, HIP 21242, HR 1434, SAO 39604, WDS J04334+4304A[9]
Database references
SIMBADdata

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. ^ a b c d e f g 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.
  2. ^ a b Høg, E.; et al. (2000), "The Tycho-2 catalogue of the 2.5 million brightest stars", Astronomy and Astrophysics, 355: L27, Bibcode:2000A&A...355L..27H, doi:10.1888/0333750888/2862.
  3. ^ a b c d Royer, F.; et al. (February 2007), "Rotational velocities of A-type stars. III. Velocity distributions", Astronomy and Astrophysics, 463 (2): 671–682, arXiv:astro-ph/0610785, Bibcode:2007A&A...463..671R, doi:10.1051/0004-6361:20065224, S2CID 18475298.
  4. ^ a b Dorrit Hoffleit (1991). Combined\bsc5: The Bright Star Catalogue. 5th Ed., Preliminary Version. Yale University Observatory.
  5. ^ a b 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.
  6. ^ 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.
  7. ^ a b c d e f g 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, arXiv:1501.03154, Bibcode:2015ApJ...804..146D, doi:10.1088/0004-637X/804/2/146, S2CID 33401607.
  8. ^ 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, arXiv:1103.4651, Bibcode:2011A&A...530A.138C, doi:10.1051/0004-6361/201016276, S2CID 56118016.
  9. ^ "57 Per". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-01-30.
  10. ^ a b c d 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.
  11. ^ Bailer-Jones, C. A. L. (March 2015), "Close encounters of the stellar kind", Astronomy & Astrophysics, 575: 13, arXiv:1412.3648, Bibcode:2015A&A...575A..35B, doi:10.1051/0004-6361/201425221, S2CID 59039482, A35.
  12. ^ a b c Mason, B. D.; et al. (2014), "The Washington Visual Double Star Catalog", The Astronomical Journal, 122 (6): 3466, Bibcode:2001AJ....122.3466M, doi:10.1086/323920
  13. ^ 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.
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