Lambda Persei

In this article, we will delve into the exciting world of Lambda Persei. We will explore its origins, its impact on today's society and the possible implications for the future. Since its appearance, Lambda Persei has captured the attention of millions of people around the world, generating debates, controversies and endless interpretations. Through a detailed analysis, we will seek to understand the importance of Lambda Persei in different areas, as well as its relevance in our daily lives. In addition, we will address different perspectives and opinions from experts in the field, in order to offer a complete and enriching vision of this fascinating topic.
Lambda Persei
Location of λ Persei (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Perseus
Right ascension 04h 06m 35.04360s[1]
Declination 50° 21′ 04.5500″[1]
Apparent magnitude (V) 4.29[2]
Characteristics
Spectral type A0IVn[3]
U−B color index −0.04[2]
B−V color index +0.02[2]
Astrometry
Radial velocity (Rv)+6.1±2.0[4] km/s
Proper motion (μ) RA: −12.75[1] mas/yr
Dec.: −35.60[1] mas/yr
Parallax (π)7.73 ± 0.22 mas[1]
Distance420 ± 10 ly
(129 ± 4 pc)
Absolute magnitude (MV)−1.31[5]
Details
Radius3.1[6] R☉
Luminosity348[5] L☉
Surface gravity (log g)4.05[7] cgs
Temperature10,585[7] K
Metallicity +0.01[7] dex
Rotational velocity (v sin i)196[8] km/s
Age345[9] Myr
Other designations
λ Per, 47 Persei, BD+49°1101, FK5 1113, GC 4924, HD 25642, HIP 19167, HR 1261, SAO 24412[10]
Database references
SIMBADdata

λ Persei, Latinized as Lambda Persei, is a star in the northern constellation of Perseus. It is visible to the naked eye as a faint, white-hued point of light with an apparent visual magnitude of 4.29.[2] This object is located approximately 422 light years from the Sun based on parallax,[1] and is drifting further away with a radial velocity of +6 km/s.[4]

λ Persei in optical light

This object has a stellar classification of A0IVn,[3] matching an A-type subgiant star with "nebulous" lines due to rapid rotation. It is spinning with a projected rotational velocity of 196 km/s,[8] which is giving the star an equatorial bulge that is an estimated 16% larger than the polar radius.[11] Unusually for a star of this type, spectra show weak emission features among the Hydrogen lines, which may be due to plage regions on the surface caused by an implied magnetic field.[12] The star is 345[9] million years old and is radiating 348[5] times the luminosity of the Sun from its photosphere at an effective temperature of 10,585 K.[7]

In Chinese astronomy, Lambda Persei is called 積水, Pinyin: Jīshuǐ, meaning Stored Water, because this star is marking itself and stand alone in Stored Water asterism, Stomach mansion (see : Chinese constellation).[13]

References

  1. ^ a b c d e f Van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. S2CID 18759600. Vizier catalog entry
  2. ^ a b c d Ducati, J. R. (2002). "Catalogue of Stellar Photometry in Johnson's 11-color system". CDS/ADC Collection of Electronic Catalogues. 2237. Bibcode:2002yCat.2237....0D.
  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 Wilson, R. E. (1953). "General Catalogue of Stellar Radial Velocities". Carnegie Institute Washington D.C. Publication. Carnegie Institution for Science. Bibcode:1953GCRV..C......0W. LCCN 54001336.
  5. ^ 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
  6. ^ Pasinetti Fracassini, L. E.; et al. (February 2001), "Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS)", Astronomy and Astrophysics, 367 (2) (Third ed.): 521–524, arXiv:astro-ph/0012289, Bibcode:2001A&A...367..521P, doi:10.1051/0004-6361:20000451, S2CID 425754
  7. ^ a b c d Wu, Yue; et al. (2010). "Coudé-feed stellar spectral library – atmospheric parameters". Astronomy & Astrophysics. 525: A71. arXiv:1009.1491. Bibcode:2011A&A...525A..71W. doi:10.1051/0004-6361/201015014. S2CID 53480665.
  8. ^ a b Hoffleit, D.; Warren, W. H. (1995). "Bright Star Catalogue". VizieR On-line Data Catalog: V/50. Originally Published in: 1964BS....C......0H. 5050 (5th Revised ed.). Bibcode:1995yCat.5050....0H.
  9. ^ a b Gontcharov, G. A. (November 2012). "Spatial distribution and kinematics of OB stars". Astronomy Letters. 38 (11): 694–706. arXiv:1606.09028. Bibcode:2012AstL...38..694G. doi:10.1134/S1063773712110035. S2CID 119108982.
  10. ^ "lam Per". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-09-22.
  11. ^ Belle, G. T. (2012). "Interferometric observations of rapidly rotating stars". The Astronomy and Astrophysics Review. 20 (1): 51. arXiv:1204.2572. Bibcode:2012A&ARv..20...51V. doi:10.1007/s00159-012-0051-2. S2CID 119273474.
  12. ^ Underhill, Anne B. (November 1991). "Lambda Persei: an Unusual B9 IV Star". Publications of the Astronomical Society of the Pacific. 103: 1176. Bibcode:1991PASP..103.1176U. doi:10.1086/132937. S2CID 121711589.
  13. ^ (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 11 日 Archived 2012-02-04 at the Wayback Machine
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