32 Persei

In today's world, 32 Persei has acquired unprecedented relevance. Whether in the field of science, technology, art, politics or everyday life, 32 Persei is a topic that has captured the attention of millions of people around the world. Its impact has been felt significantly in our lives, generating debates, controversies and discoveries that have transformed our perception and understanding of 32 Persei. In this article, we will explore this phenomenon in depth, analyzing its various facets, its history, its current influence and its future potential.
This article is about l Persei. Not to be confused with i Persei or ι (iota) Persei.
32 Persei
Location of 32 Persei (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Perseus
Right ascension 03h 21m 26.55723s[1]
Declination 43° 19′ 46.7414″[1]
Apparent magnitude (V) 4.96[2]
Characteristics
Spectral type A3V[3]
U−B color index +0.07[4]
B−V color index +0.04[4]
Astrometry
Radial velocity (Rv)−9.00[5] km/s
Proper motion (μ) RA: −59.947[1] mas/yr
Dec.: −0.839[1] mas/yr
Parallax (π)21.8865 ± 0.2690 mas[1]
Distance149 ± 2 ly
(45.7 ± 0.6 pc)
Absolute magnitude (MV)1.64[2]
Details
Mass2.05[6] M☉
Radius1.8[7] R☉
Luminosity21[6] L☉
Surface gravity (log g)4.19[8] cgs
Temperature8,872[6] K
Metallicity −0.01[9] dex
Rotational velocity (v sin i)144[6] km/s
Age125+75
−25[10] Myr
Other designations
l Per, 32 Per, NSV 1107, BD+42°750, FK5 2236, GC 4004, HD 20677, HIP 15648, HR 1002, SAO 38750[11]
Database references
SIMBADdata

32 Persei is a single[12] star located 149[1] light years away from the Sun in the northern constellation of Perseus.[11] It has the Bayer designation of l Persei, while 32 Persei is the Flamsteed designation. This object is visible to the naked eye as a faint, white-hued star with an apparent visual magnitude of 4.96.[2] It is moving closer to the Earth with a heliocentric radial velocity of −9 km/s,[5] and is a member of the Sirius supercluster: a stream of stars that share a common motion through space.[13]

This is an ordinary A-type main-sequence star with a stellar classification of A3V.[3] It is around 125[10] million years old with a high rate of spin, showing a projected rotational velocity of 144 km/s.[6] The star has double[6] the mass of the Sun and 1.8[7] times the Sun's radius. It is radiating 21[6] times the luminosity of the Sun from its photosphere at an effective temperature of 8,872 K.[6]

References

  1. ^ a b c d e f Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  2. ^ a b c 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. Vizier catalog entry
  3. ^ a b Cowley, A.; et al. (April 1969). "A study of the bright A stars. I. A catalogue of spectral classifications". Astronomical Journal. 74: 375–406. Bibcode:1969AJ.....74..375C. doi:10.1086/110819.
  4. ^ a b Mallama, A. (2014). "Sloan Magnitudes for the Brightest Stars". The Journal of the American Association of Variable Star Observers. 42 (2): 443. Bibcode:2014JAVSO..42..443M.Vizier catalog entry
  5. ^ a b Gontcharov, G. A. (2006). "Pulkovo Compilation of Radial Velocities for 35 495 Hipparcos stars in a common system". Astronomy Letters. 32 (11): 759–771. arXiv:1606.08053. Bibcode:2006AstL...32..759G. doi:10.1134/S1063773706110065. S2CID 119231169.
  6. ^ a b c d e f g h Zorec, J.; Royer, F. (2012). "Rotational velocities of A-type stars". Astronomy & Astrophysics. 537: A120. arXiv:1201.2052. Bibcode:2012A&A...537A.120Z. doi:10.1051/0004-6361/201117691. S2CID 55586789. Vizier catalog entry
  7. ^ a b Allende Prieto, C.; Lambert, D. L. (1999). "Fundamental parameters of nearby stars from the comparison with evolutionary calculations: Masses, radii and effective temperatures". Astronomy and Astrophysics. 352: 555–562. arXiv:astro-ph/9911002. Bibcode:1999A&A...352..555A. Vizier catalog entry
  8. ^ 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. Vizier catalog entry
  9. ^ Gontcharov, G. A. (2012). "Dependence of kinematics on the age of stars in the solar neighborhood". Astronomy Letters. 38 (12): 771–782. arXiv:1606.08814. Bibcode:2012AstL...38..771G. doi:10.1134/S1063773712120031. S2CID 118345778. Vizier catalog entry
  10. ^ a b Meshkat, Tiffany; et al. (December 2017). "A Direct Imaging Survey of Spitzer-detected Debris Disks: Occurrence of Giant Planets in Dusty Systems". The Astronomical Journal. 154 (6): 21. arXiv:1710.04185. Bibcode:2017AJ....154..245M. doi:10.3847/1538-3881/aa8e9a. S2CID 42042014. 245.
  11. ^ a b "32 Per". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-07-10.
  12. ^ Eggleton, P. P.; Tokovinin, A. A. (2008). "A catalogue of multiplicity among bright stellar systems". Monthly Notices of the Royal Astronomical Society. 389 (2): 869. arXiv:0806.2878. Bibcode:2008MNRAS.389..869E. doi:10.1111/j.1365-2966.2008.13596.x. S2CID 14878976.
  13. ^ Palous, J.; Hauck, B. (July 1986), "The Sirius supercluster", Astronomy and Astrophysics, 162: 54–61, Bibcode:1986A&A...162...54P.
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