HD 120565

Spectroscopic binary in the constellation Camelopardalis
HD 120565
Location of HD 120565 on the map (circled)
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Camelopardalis
Right ascension 13h 42m 23.18342s[1]
Declination +82° 45′ 08.7103″[1]
Apparent magnitude (V) 5.91±0.01[2]
Characteristics
Spectral type G9 III[3]
B−V color index +1.01[4]
Astrometry
Radial velocity (Rv)−45.2±1.2[5] km/s
Proper motion (μ) RA: +29.995 mas/yr[1]
Dec.: −43.734 mas/yr[1]
Parallax (π)8.8109 ± 0.0364 mas[1]
Distance370 ± 2 ly
(113.5 ± 0.5 pc)
Absolute magnitude (MV)+0.48[6]
Details
Mass2.70±0.11[1] M☉
Radius10.8+0.3
−0.2[7] R☉
Luminosity64.1±0.5[1] L☉
Surface gravity (log g)2.47[8] cgs
Temperature4,993±122[9] K
Metallicity [Fe/H]−0.20[10] dex
Rotational velocity (v sin i)2.6±1[11] km/s
Age503+75
−70[1] Myr
Other designations
AG+83°357, BD+83°397, FK5 1643, GC 18611, HD 120565, HIP 66878, HR 5203, SAO 2266[12]
Database references
SIMBADdata

HD 120565, also designated as HR 5203, is a star located in the northern circumpolar constellation Camelopardalis. It is faintly visible to the naked eye as an orange-hued point of light with an apparent magnitude of 5.91. Gaia DR3 parallax measurements imply a distance of 370 light-years and it is currently drifting closer with a heliocentric radial velocity of −45.2 km/s. At its current distance, HD 120565's brightness is diminished by 0.12 magnitudes due to interstellar extinction[13] and it has an absolute magnitude of +0.48.[6]

HD 120565 has a stellar classification of G9 III,[3] indicating that it is an evolved G-type giant star. It has 2.7 times the mass of the Sun[1] but at the age of 503 million years,[1] it has expanded to 10.8 times the radius of the Sun.[7] It radiates 64.1 times the luminosity of the Sun[1] from its enlarged photosphere at an effective temperature of 4,993 K.[9] HD 120565 is metal deficient with an iron abundance 63.1% that of the Sun's or [Fe/H] = −0.22,[10] and it spins modestly with a projected rotational velocity of 2.6 km/s.[11] It was determined to be a single-lined spectroscopic binary by J.R. De Mederios and J. R. P. da Silva based on radial velocity variations.[11]

References

  1. ^ a b c d e f g h i j Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
  2. ^ Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P.; Wicenec, A. (March 2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics. 355: L27–L30. Bibcode:2000A&A...355L..27H. ISSN 0004-6361. S2CID 17128864.
  3. ^ a b Cowley, A. P.; Bidelman, W. P. (February 1979). "MK spectral types for some F and G stars". Publications of the Astronomical Society of the Pacific. 91: 83. Bibcode:1979PASP...91...83C. doi:10.1086/130446. eISSN 1538-3873. ISSN 0004-6280.
  4. ^ Haggkvist, L.; Oja, T. (1970). "Results of BV photometry 1969-70 (Uppsala refractor)". Private Communication. Bibcode:1970Priv.........0H. S2CID 231475662.
  5. ^ Gontcharov, G. A. (November 2006). "Pulkovo Compilation of Radial Velocities for 35,495 Hipparcos stars in a common system". Astronomy Letters. 32 (11): 759–771. arXiv:1606.08053. Bibcode:2006AstL...32..759G. doi:10.1134/S1063773706110065. eISSN 1562-6873. ISSN 1063-7737. S2CID 119231169.
  6. ^ a b Anderson, E.; Francis, Ch. (May 2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331–346. arXiv:1108.4971. Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. eISSN 1562-6873. ISSN 1063-7737. S2CID 119257644.
  7. ^ a b 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.
  8. ^ Anders, F.; et al. (August 2019). "Photo-astrometric distances, extinctions, and astrophysical parameters for Gaia DR2 stars brighter than G = 18". Astronomy & Astrophysics. 628: A94. arXiv:1904.11302. Bibcode:2019A&A...628A..94A. doi:10.1051/0004-6361/201935765. eISSN 1432-0746. ISSN 0004-6361. S2CID 131780028.
  9. ^ a b Stassun, Keivan G.; et al. (9 September 2019). "The Revised TESS Input Catalog and Candidate Target List". The Astronomical Journal. 158 (4): 138. arXiv:1905.10694. Bibcode:2019AJ....158..138S. doi:10.3847/1538-3881/ab3467. eISSN 1538-3881. hdl:1721.1/124721. S2CID 166227927.
  10. ^ a b Charbonnel, C.; Lagarde, N.; Jasniewicz, G.; North, P. L.; Shetrone, M.; Krugler Hollek, J.; Smith, V. V.; Smiljanic, R.; Palacios, A.; Ottoni, G. (January 2020). "Lithium in red giant stars: Constraining non-standard mixing with large surveys in the Gaia era". Astronomy & Astrophysics. 633: A34. arXiv:1910.12732. Bibcode:2020A&A...633A..34C. doi:10.1051/0004-6361/201936360. eISSN 1432-0746. ISSN 0004-6361. S2CID 204907220.
  11. ^ a b c De Medeiros, J. R.; Da Silva, J. R. P.; Maia, M. R. G. (20 October 2002). "The Rotation of Binary Systems with Evolved Components". The Astrophysical Journal. 578 (2): 943–950. arXiv:astro-ph/0207288. Bibcode:2002ApJ...578..943D. doi:10.1086/342613. eISSN 1538-4357. ISSN 0004-637X. S2CID 16196039.
  12. ^ "HD 120565". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved August 22, 2023.
  13. ^ Gontcharov, George A.; Mosenkov, Aleksandr V. (28 September 2017). "Verifying reddening and extinction for Gaia DR1 TGAS main sequence stars". Monthly Notices of the Royal Astronomical Society. 472 (4): 3805–3820. arXiv:1709.01160. Bibcode:2017MNRAS.472.3805G. doi:10.1093/mnras/stx2219. eISSN 1365-2966. ISSN 0035-8711. S2CID 118879856.
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