52 Hydrae

In today's world, 52 Hydrae is a topic that has become increasingly relevant. Both on a personal and professional level, 52 Hydrae has captured the attention of a large number of individuals and has generated debate in different sectors. Over time, opinions and perspectives on 52 Hydrae have evolved, resulting in a growing interest in fully understanding its importance and impact on society. In this article, we will explore in detail the various facets of 52 Hydrae, analyzing its impact in different contexts and offering a comprehensive vision that allows us to fully understand its relevance in today's world.

This article is about l Hydrae. Not to be confused with I Hydrae, ι (iota) Hydrae, or λ (lambda) Hydrae.
52 Hydrae
Observation data
Epoch J2000      Equinox J2000
Constellation Hydra
Right ascension 14h 28m 10.42638s[1]
Declination −29° 29′ 29.8884″[1]
Apparent magnitude (V) 4.97[2] (5.70 + 5.70 + 10.00)[3]
Characteristics
Evolutionary stage main sequence[4]
Spectral type B7/8V[5]
B−V color index −0.074±0.003[2]
Astrometry
Radial velocity (Rv)5.4±3.8[2] km/s
Proper motion (μ) RA: −25.23[1] mas/yr
Dec.: −23.03[1] mas/yr
Parallax (π)8.29±0.28 mas[1]
Distance390 ± 10 ly
(121 ± 4 pc)
Absolute magnitude (MV)−0.43[2]
Details
52 Hya A
Mass3.82±0.06[4] M☉
Luminosity310.5+24.5
−22.8[4] L☉
Temperature12,853±89[4] K
Rotational velocity (v sin i)204[4] km/s
Other designations
l Hya, 52 Hya, CD−28°10712, FK5 532, HD 126769, HIP 70753, HR 5407, SAO 182570, ADS 9270, WDS J14282-2929[6]
Database references
SIMBADdata

52 Hydrae is a triple star system[7] in the constellation Hydra. It has the Bayer designation l Hydrae; 52 Hydrae is the Flamsteed designation.[6] This system is visible to the naked eye as a faint, blue-white hued star with an apparent visual magnitude of 4.97.[2] It is a probable (80% chance) member of the Sco OB2 moving group of stars,[8] and is moving away from the Earth with a heliocentric radial velocity of 5 km/s.[2]

The primary component is a binary system[7] consisting of two nearly equal components with an orbital period of around 15 years[9] and an angular separation of 0.1″.[7] It shows a combined stellar classification of B7/8V,[5] which matches a B-type main-sequence star. The third component is a magnitude 10.0 star at a separation of 4.2″[7] with a mass similar to the Sun. It is orbiting the inner pair with a period of around 3,900 years.[9]

References

  1. ^ a b c d e 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.
  2. ^ a b c d e f 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. ^ Mason, B. D.; et al. (2014), "The Washington Visual Double Star Catalog", The Astronomical Journal, 122 (6): 3466, Bibcode:2001AJ....122.3466M, doi:10.1086/323920, retrieved 2015-07-22.
  4. ^ a b c d e Zorec, J.; Royer, F. (2012), "Rotational velocities of A-type stars. IV. Evolution of rotational velocities", Astronomy & Astrophysics, 537: A120, arXiv:1201.2052, Bibcode:2012A&A...537A.120Z, doi:10.1051/0004-6361/201117691, S2CID 55586789.
  5. ^ a b Houk, Nancy (1979), Michigan catalogue of two-dimensional spectral types for the HD stars, vol. 3, Ann Arbor, Michigan: Dept. of Astronomy, University of Michigan, Bibcode:1982mcts.book.....H.
  6. ^ a b "l Hya". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved May 5, 2019.
  7. ^ a b c d 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.
  8. ^ Rizzuto, Aaron; et al. (October 2011), "Multidimensional Bayesian membership analysis of the Sco OB2 moving group", Monthly Notices of the Royal Astronomical Society, 416 (4): 3108–3117, arXiv:1106.2857, Bibcode:2011MNRAS.416.3108R, doi:10.1111/j.1365-2966.2011.19256.x, S2CID 54510608.
  9. ^ a b Tokovinin, A. (September 2008), "Comparative statistics and origin of triple and quadruple stars", Monthly Notices of the Royal Astronomical Society, 389 (2): 925–938, arXiv:0806.3263, Bibcode:2008MNRAS.389..925T, doi:10.1111/j.1365-2966.2008.13613.x, S2CID 16452670.