Astronomy:53 Persei

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Short description: Star in the constellation Perseus
53 Persei
Perseus constellation map.svg
Red circle.svg
Location of 53 Persei (circled)
Observation data
Equinox J2000.0]] (ICRS)
Constellation Perseus
Right ascension  04h 21m 33.16651s[1]
Declination 46° 29′ 55.9591″[1]
Apparent magnitude (V) 4.80[2]
Characteristics
Spectral type B4IV[3]
U−B color index −0.52[4]
B−V color index −0.03[4]
Variable type SPB[5]
Astrometry
Radial velocity (Rv)+7.30[6] km/s
Proper motion (μ) RA: +21.482[1] mas/yr
Dec.: −34.832[1] mas/yr
Parallax (π)6.8517 ± 0.2700[1] mas
Distance480 ± 20 ly
(146 ± 6 pc)
Absolute magnitude (MV)−1.42[7]
Details
Mass5.9±0.1[8] M☉
Radius3.98±0.49[7] R☉
Luminosity779.8+213.3
−167.5[7] L☉
Surface gravity (log g)3.93±0.09[7] cgs
Temperature16,720[9] K
Rotational velocity (v sin i)15[10] km/s
Age50.1±9.3[8] Myr
Other designations
d Per, 53 Per, V469 Per, NSV 1560, BD+46°872, FK5 2319, GC 5256, HD 27396, HIP 20354, HR 1350, SAO 39483[11]
Database references
SIMBADdata

53 Persei is a single[12] variable star in the northern constellation of Perseus. It has the Bayer designation d Persei, while 53 Persei is the Flamsteed designation. The star is visible to the naked eye as a faint, blue-white hued point of light with an apparent visual magnitude of 4.80.[2] It is located approximately 480 light years away from the Sun, as determined from parallax, and is drifting further away with a radial velocity of +7.3 km/s.[6]

A visual band light curve for V469 Persei, plotted from data published by Huang et al. (1994)[13]

This star has a stellar classification of B4IV,[3] and was the prototype of a class of variable stars known as slowly pulsating B stars.[14] It was one of the first mid-B type variable stars in the northern hemisphere to be studied.[5] The star undergoes non-radial pulsations with a primary period of 2.36 days. Observation of the star with the BRITE satellite revealed eight separate frequencies in the star's light curve.[5]

53 Persei is around 50[8] million years old with a projected rotational velocity of 15 km/s.[10] It has six[8] times the mass of the Sun and four[7] times the Sun's radius. The star is radiating 780[7] times the luminosity of the Sun from its photosphere at an effective temperature of 16,720 K.[9]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G.  Gaia DR2 record for this source at VizieR.
  2. ↑ 2.0 2.1 Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters 38 (5): 331. doi:10.1134/S1063773712050015. Bibcode: 2012AstL...38..331A.  Vizier catalog entry
  3. ↑ 3.0 3.1 Lesh, Janet Rountree (1968). "The Kinematics of the Gould Belt: An Expanding Group?". Astrophysical Journal Supplement 17: 371. doi:10.1086/190179. Bibcode: 1968ApJS...17..371L. 
  4. ↑ 4.0 4.1 Mermilliod, J. C. (2006). "VizieR Online Data Catalog: Homogeneous Means in the UBV System (Mermilliod 1991)". VizieR On-line Data Catalog: II/168. Originally Published in: Institut d'Astronomie 2168. Bibcode: 2006yCat.2168....0M. Vizier catalog entry
  5. ↑ 5.0 5.1 5.2 Niemczura, E.; Pigulski, A.; Lehmann, H.; Kamiński, K.; Catanzaro, G.; Stateva, I.; Napetova, M. (September 2017). "Photometric and spectroscopic variability of 53 Per". in Zwintz, Konnstanze; Poretti, Ennio. Second BRITE-Constellation Science Conference: Small satellites—big science, held 22–26 August 2016 in Innsbruck, Austria. 5. Warsaw, Poland: Polish Astronomical Society. pp. 217–218. Bibcode: 2017sbcs.conf..217N. 
  6. ↑ 6.0 6.1 Gontcharov, G. A. (2006). "Pulkovo Compilation of Radial Velocities for 35 495 Hipparcos stars in a common system". Astronomy Letters 32 (11): 759–771. doi:10.1134/S1063773706110065. Bibcode: 2006AstL...32..759G. 
  7. ↑ 7.0 7.1 7.2 7.3 7.4 7.5 Briquet, M. et al. (April 2007). "On the co-existence of chemically peculiar Bp stars, slowly pulsating B stars and constant B stars in the same part of the HR diagram". Astronomy and Astrophysics 466 (1): 269–276. doi:10.1051/0004-6361:20066940. Bibcode: 2007A&A...466..269B. 
  8. ↑ 8.0 8.1 8.2 8.3 Tetzlaff, N. et al. (2011). "A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun". Monthly Notices of the Royal Astronomical Society 410 (1): 190–200. doi:10.1111/j.1365-2966.2010.17434.x. Bibcode: 2011MNRAS.410..190T.  Vizier catalog entry
  9. ↑ 9.0 9.1 Zorec, J. et al. (2009). "Fundamental parameters of B supergiants from the BCD system". Astronomy and Astrophysics 501: 297–320. doi:10.1051/0004-6361/200811147. Bibcode: 2009A&A...501..297Z. 
  10. ↑ 10.0 10.1 Abt, Helmut A. et al. (2002). "Rotational Velocities of B Stars". The Astrophysical Journal 573 (1): 359–365. doi:10.1086/340590. Bibcode: 2002ApJ...573..359A. 
  11. ↑ "53 Per". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=53+Per. 
  12. ↑ 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. 
  13. ↑ Huang, L.; Guo, Z.; Hao, J.; Percy, J. R.; Fieldus, M. S.; Fried, R.; Pavlovski, K.; Bozic, H. et al. (August 1994). "A Multisite UBV Photometric Campaign on 53 Persei in 1991 January". The Astrophysical Journal 431: 850–869. doi:10.1086/174536. Bibcode: 1994ApJ...431..850H. https://ui.adsabs.harvard.edu/abs/1994ApJ...431..850H. Retrieved 16 February 2022. 
  14. ↑ Le Contel, J. M. et al. (1989). "Spectral variations in 53 Per". Acta Astronomica 39 (3): 227–234. Bibcode: 1989AcA....39..227L. 



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