HD 96566

In the contemporary world, HD 96566 has gained unprecedented relevance. Whether due to its impact on society, its role in popular culture or its relevance in academia, HD 96566 has become a recurring topic of conversation. In fact, it is not surprising that HD 96566 is the subject of debate and analysis in numerous areas, since its influence extends to multiple aspects of modern life. In this article we will explore the HD 96566 phenomenon in depth, addressing its various facets and analyzing its importance in the current context.

For other stars with the Bayer designation z Carinae, see z Carinae.
HD 96566
Observation data
Epoch J2000      Equinox J2000
Constellation Carina
Right ascension 11h 06m 32.42668s[1]
Declination −62° 25′ 26.8119″[1]
Apparent magnitude (V) +4.62[2]
Characteristics
Spectral type G7.5III[3]
B−V color index 0.988±0.065[2]
Astrometry
Radial velocity (Rv)−1.07±0.17[1] km/s
Proper motion (μ) RA: −36.93±0.16[4] mas/yr
Dec.: +9.46±0.14[4] mas/yr
Parallax (π)8.6750±0.1387 mas[1]
Distance376 ± 6 ly
(115 ± 2 pc)
Absolute magnitude (MV)−0.81[2]
Details
Mass3.6[5] M☉
Radius20.21+0.36
−0.39[1] R☉
Luminosity214.4±4.0[1] L☉
Surface gravity (log g)2.59±0.17[6] cgs
Temperature4,913+49
−43[1] K
Metallicity 0.05±0.05[6] dex
Other designations
z1 Carinae, CPD−61°2067, GC 15288, GJ 9345, HD 96566, HIP 54301, HR 4325, SAO 251269[7]
Database references
SIMBADdata

HD 96566 is a single[8] star in the southern constellation of Carina. It has the Bayer designation z1 Carinae; HD 96566 is the identifier from the Henry Draper Catalogue. This object has a yellow hue and is visible to the naked eye with an apparent visual magnitude of +4.62.[2] The star is located at a distance of approximately 376 light years from the Sun based on parallax, but is drifting closer with a radial velocity of −1 km/s.[1] It has an absolute magnitude of −0.81.[2]

This is an aging G-type giant star with a stellar classification of G7.5III,[3] which indicates it has exhausted the supply of hydrogen at its core then cooled and expanded off the main sequence. It has an estimated 3.6[5] times the mass of the Sun and has grown to 20[1] times the Sun's radius. The metallicity, or abundance of elements other than hydrogen and helium, is about the same as in the Sun.[6] It is radiating about 214[1] times the Sun's luminosity from its photosphere at an effective temperature of 4,913 K.[1]

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 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 Keenan, Philip C.; McNeil, Raymond C. (1989). "The Perkins catalog of revised MK types for the cooler stars". Astrophysical Journal Supplement Series. 71: 245. Bibcode:1989ApJS...71..245K. doi:10.1086/191373.
  4. ^ a b 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.
  5. ^ a b Gondoin, P. (December 1999), "Evolution of X-ray activity and rotation on G-K giants", Astronomy and Astrophysics, 352: 217–227, Bibcode:1999A&A...352..217G.
  6. ^ a b c Alves, S.; et al. (April 2015), "Determination of the spectroscopic stellar parameters for 257 field giant stars", Monthly Notices of the Royal Astronomical Society, 448 (3): 2749–2765, arXiv:1503.02556, Bibcode:2015MNRAS.448.2749A, doi:10.1093/mnras/stv189.
  7. ^ "HD 96566". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-07-11.
  8. ^ 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.