11 Persei

In this article we are going to talk about 11 Persei, a topic that has been the subject of great interest and debate in recent years. 11 Persei has captured the attention of academics, professionals and enthusiasts alike, and it is not surprising, given its impact on aspects as diverse as society, culture, technology and the economy. Over the next few lines, we will explore the various aspects of 11 Persei, from its origins to its current influence, unraveling its complexities and offering a comprehensive view of this fascinating topic. We are confident that by the end of this article, you will have gained a deeper knowledge and appreciation of 11 Persei.

11 Persei
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Perseus
Right ascension 02h 43m 02.83826s[1]
Declination +55° 06′ 21.6700″[1]
Apparent magnitude (V) 5.76[2]
Characteristics
Evolutionary stage main sequence[3]
Spectral type B7 III(p?) (Hg?)[4]
B−V color index −0.110±0.003[2]
Astrometry
Radial velocity (Rv)−0.7±1.0[2] km/s
Proper motion (μ) RA: +34.859[1] mas/yr
Dec.: −21.955[1] mas/yr
Parallax (π)7.8022 ± 0.0874 mas[1]
Distance418 ± 5 ly
(128 ± 1 pc)
Absolute magnitude (MV)0.16[2]
Details
Mass3.77±0.06[3] M☉
Radius3.2[5] R☉
Luminosity210.4+21.9
−19.9[3] L☉
Surface gravity (log g)4.19[6] cgs
Temperature14,550[6] K
Metallicity +0.09[6] dex
Rotation25–70 d[7]
Rotational velocity (v sin i)4.50[8] km/s
Age50.9±12.2[9] Myr
Other designations
11 Per, BD+54°598, FK5 2188, HD 16727, HIP 12692, HR 785, SAO 23555[10]
Database references
SIMBADdata

11 Persei is a single[11][8] star in the constellation of Perseus, located about 418 light years away from the Sun. It is visible to the naked eye as a dim, blue-white hued star with an apparent visual magnitude of 5.76.[2]

This is a chemically peculiar mercury-manganese star.[12][6] Cowley (1972) found a stellar classification of B7 III(p?) (Hg?),[4] while Hube (1970) had B8 IV,[13] and Appenzeller (1967) showed B6 V.[14] Stellar models indicate this is a young B-type main sequence star[3] with an estimated age of around 51[9] million years. It has a low rotation rate, showing a projected rotational velocity of 4.50 km/s.[8] The star has 3.8[3] times the mass of the Sun and is radiating 210[3] times the Sun's luminosity from its photosphere at an effective temperature of 14,550 K.[6]

References

  1. ^ a b c d e 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 d e 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.
  3. ^ a b c d e f Zorec, J.; Royer, F.; Asplund, Martin; Cassisi, Santi; Ramirez, Ivan; Melendez, Jorge; Bensby, Thomas; Feltzing, Sofia (2012), "Rotational velocities of A-type stars. IV. Evolution of rotational velocities", Astronomy and Astrophysics, 537: A120, arXiv:1201.2052, Bibcode:2012A&A...537A.120Z, doi:10.1051/0004-6361/201117691, S2CID 55586789.
  4. ^ a b Cowley, A. (November 1972), "Spectral classification of the bright B8 stars", Astronomical Journal, 77: 750–755, Bibcode:1972AJ.....77..750C, doi:10.1086/111348.
  5. ^ Pasinetti Fracassini, L. E.; et al. (February 2001), "Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS)", Astronomy and Astrophysics, 367 (Third ed.): 521–524, arXiv:astro-ph/0012289, Bibcode:2001A&A...367..521P, doi:10.1051/0004-6361:20000451, S2CID 425754.
  6. ^ a b c d e Ghazaryan, S.; Alecian, G. (2016), "Statistical analysis from recent abundance determinations in HgMn stars", Monthly Notices of the Royal Astronomical Society, 460 (2): 1912, Bibcode:2016MNRAS.460.1912G, doi:10.1093/mnras/stw911.
  7. ^ Wahlgren, Glenn Michael; et al. (January 2012), "Emission Line Variability In The HgMn Star 11 Per", American Astronomical Society, AAS Meeting #219, vol. 219, p. 439.04, Bibcode:2012AAS...21943904W, 439.04.
  8. ^ a b c Hubrig, S.; Castelli, F. (September 2001), "New results of magnetic field diagnosis in HgMn stars and normal late B-type stars", Astronomy and Astrophysics, 375 (3): 963–976, Bibcode:2001A&A...375..963H, doi:10.1051/0004-6361:20010894.
  9. ^ a b Tetzlaff, N.; et al. (January 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, arXiv:1007.4883, Bibcode:2011MNRAS.410..190T, doi:10.1111/j.1365-2966.2010.17434.x, S2CID 118629873.
  10. ^ "11 Per". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-03-28.
  11. ^ 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.
  12. ^ Adelman, S. J.; Yüce, K. (August 2010), "Elemental abundance analyses with Coudé Echelle spectrograms from the TÜBİTAK National Observatory of Turkey: I. The HgMn stars 11 Per, HR 2801, and ν Cnc", Astronomische Nachrichten, 331 (8): 785–793, Bibcode:2010AN....331..785A, doi:10.1002/asna.201011411.
  13. ^ Hube, Douglas P. (1970), "The radial velocities of 335 late B-type stars", Memoirs of the Royal Astronomical Society, 72: 233–280, Bibcode:1970MmRAS..72..233H.
  14. ^ Appenzeller, Immo (April 1967), "MK Spectral Types for 185 Bright Stars", Publications of the Astronomical Society of the Pacific, 79 (467): 102, Bibcode:1967PASP...79..102A, doi:10.1086/128449.