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Lambda Horologii

In today's world, Lambda Horologii has become a topic of great importance and interest to a wide variety of people. From its impact on society to its relevance in politics and economics, Lambda Horologii has managed to capture the attention of experts and fans alike. Whether due to its influence on popular culture or its significance in the academic field, Lambda Horologii has generated a debate in which individuals of all ages and backgrounds actively participate. As Lambda Horologii continues to evolve and take on new nuances, the need to understand it in all its complexity becomes even more evident. In this article, we will explore various facets of Lambda Horologii and its impact on contemporary society.

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Lambda Horologii
Observation data
Epoch J2000      Equinox J2000
Constellation Horologium
Right ascension 02h 24m 53.91034s[1]
Declination −60° 18′ 43.0170″[1]
Apparent magnitude (V) +5.35[2]
Characteristics
Spectral type F2III[3]
B−V color index +0.39[2]
Astrometry
Radial velocity (Rv)+28.34±0.41[1] km/s
Proper motion (μ) RA: −71.892[1] mas/yr
Dec.: −131.088[1] mas/yr
Parallax (π)21.0119±0.1004 mas[1]
Distance155.2 ± 0.7 ly
(47.6 ± 0.2 pc)
Absolute magnitude (MV)+1.91[4]
Details
Mass1.76[5] M☉
Radius2.74+0.11
−0.16[1] R☉
Luminosity13.3±0.1[1] L☉
Surface gravity (log g)3.66[6] cgs
Temperature6,848[5] K
Metallicity −0.12[5] dex
Rotational velocity (v sin i)+140[3] km/s
Age1.4[5] Gyr
Other designations
λ Hor, CPD−60°199, FK5 84, HD 15233, HIP 11258, HR 714, SAO 248555[7]
Database references
SIMBADdata

λ Horologii, Latinised as Lambda Horologii, is a star in the southern constellation of Horologium. It is a yellow-white hued star that is dimly visible to the naked eye with an apparent visual magnitude of +5.35.[2] Based upon parallax, this object is located 155 light years distance from the Sun. It is drifting further away with a radial velocity of +28 km/s.[1] Although Eggleton and Tokovinin (2008) list this as a single star,[8] according to Kunzli and North (1998) it may be a binary system with a long orbital period.[9]

The visible component has a stellar classification of F2III,[3] matching an evolved star that has, at the age of 1.4 billion years,[5] become a giant. However, it has just 2.74[1] times the Sun's radius and shows a high rate of spin with a projected rotational velocity of +140 km/s.[3] The star has 1.76[5] times the mass of the Sun and is radiating 13[1] times the Sun's luminosity from its photosphere at an effective temperature of 6,848 K.[5]

References

  1. ^ a b c d e f g h i j k 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 Johnson, H. L.; et al. (1966), "UBVRIJKL photometry of the bright stars", Communications of the Lunar and Planetary Laboratory, 4 (99), Bibcode:1966CoLPL...4...99J.
  3. ^ a b c d 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.
  4. ^ Ammler-von Eiff, Matthias; Reiners, Ansgar (June 2012), "New measurements of rotation and differential rotation in A-F stars: are there two populations of differentially rotating stars?", Astronomy & Astrophysics, 542: A116, arXiv:1204.2459, Bibcode:2012A&A...542A.116A, doi:10.1051/0004-6361/201118724, S2CID 53666672.
  5. ^ a b c d e f g Casagrande, L.; et al. (2011). "New constraints on the chemical evolution of the solar neighbourhood and Galactic disc(s). Improved astrophysical parameters for the Geneva-Copenhagen Survey". Astronomy & Astrophysics. 530 (A138): 21. arXiv:1103.4651. Bibcode:2011A&A...530A.138C. doi:10.1051/0004-6361/201016276. S2CID 56118016.
  6. ^ 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.
  7. ^ "Lam Hor". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 20 March 2016.
  8. ^ 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.
  9. ^ Kunzli, M.; North, P. (January 1998). "Are metallic A-F giants evolved AM stars? Rotation and rate of binaries among giant F stars". Astronomy and Astrophysics Supplement. 127 (2): 277–294. arXiv:astro-ph/9710226. Bibcode:1998A&AS..127..277K. doi:10.1051/aas:1998350. S2CID 7535170.
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