Astronomy:HD 26755

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Short description: Binary star system in Camelopardalis
HD 26755
Location of HD 26755 on the map (circled)
Observation data
Epoch J2000.0   Equinox (celestial coordinates)
Constellation Camelopardalis[1]
Right ascension  04h 17m 08.09353s[2]
Declination +57° 51′ 37.1513″[2]
Apparent magnitude (V) 5.72±0.01[3]
Characteristics
Evolutionary stage red clump[4]
Spectral type K1 III[5]
B−V color index +1.09[6]
Astrometry
Radial velocity (Rv)−38.2±1.6[7] km/s
Proper motion (μ) RA: +29.108[2] mas/yr
Dec.: −25.942[2] mas/yr
Parallax (π)12.0207 ± 0.1939[2] mas
Distance271 ± 4 ly
(83 ± 1 pc)
Absolute magnitude (MV)+1.21[1]
Orbit[8]
PrimaryA
CompanionB
Period (P)1,658.7±2.9 d
Eccentricity (e)0.309±0.005
Periastron epoch (T)2,453,848±5 JD
Argument of periastron (ω)
(secondary)		31.2±1.2°
Semi-amplitude (K1)
(primary)		6.10±0.04 km/s
Details
Mass1.68[9] M☉
Radius9.44±0.47[10] R☉
Luminosity42.5±1.3[2] L☉
Surface gravity (log g)2.58±0.11[11] cgs
Temperature4,717±92[11] K
Metallicity [Fe/H]+0.17±0.05[11] dex
Rotational velocity (v sin i)1±1[12] km/s
Age2.13[9] Gyr
Other designations
BD+57°787, GC 5139, HD 26755, HIP 19983, HR 1313, SAO 24514[13]
Database references
SIMBADdata

HD 26755, also known as HR 1313, is a spectroscopic binary[12][14] located in the northern circumpolar constellation Camelopardalis, the giraffe. It has an apparent magnitude of 5.72,[3] making it faintly visible to the naked eye under ideal conditions. Gaia DR3 parallax measurements place the system at a distance of 271 light years[2] and is currently drifting closer with a heliocentric radial velocity of −38 km/s.[7] At its current distance, HD 26755's brightness is diminished by 0.19 magnitudes due to interstellar dust.[15]

The visible component is an evolved red giant with a stellar classification of K1 III.[5] It is estimated to be 2.13 billion years old,[9] enough time for the star to exhaust its core hydrogen and evolve to become a red giant. It has cooled and expanded to 9.4 times the Sun's radius. It has 1.68 times the mass of the Sun[9] and radiates 42.5 times the luminosity of the Sun[2] from its enlarged photosphere at an effective temperature of 4,717 K,[11] giving it an orange hue when viewed in the night sky. HD 26755 is a metal enriched star with an iron abundance 48% greater than the Sun.[11] It spins slowly with a projected rotational velocity of 1 km/s,[12] which is poorly constrained.

References

  1. ↑ 1.0 1.1 Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters 38 (5): 331. doi:10.1134/S1063773712050015. Bibcode: 2012AstL...38..331A  XHIP record for this object at VizieR.
  2. ↑ 2.0 2.1 2.2 2.3 2.4 2.5 2.6 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940  Gaia DR3 record for this source at VizieR.
  3. ↑ 3.0 3.1 Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P. et al. (March 2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics 355: L27–L30. ISSN 0004-6361. Bibcode: 2000A&A...355L..27H. 
  4. ↑ Mishenina, T. V.; Bienaymé, O.; Gorbaneva, T. I.; Charbonnel, C.; Soubiran, C.; Korotin, S. A.; Kovtyukh, V. V. (2006). "Elemental abundances in the atmosphere of clump giants". Astronomy and Astrophysics 456 (3): 1109. doi:10.1051/0004-6361:20065141. Bibcode: 2006A&A...456.1109M. 
  5. ↑ 5.0 5.1 Appenzeller, Immo (April 1967). "MK Spectral Types for 185 Bright Stars". Publications of the Astronomical Society of the Pacific 79 (467): 102. doi:10.1086/128449. ISSN 0004-6280. Bibcode: 1967PASP...79..102A. 
  6. ↑ Haggkvist, L.; Oja, T. (1970). "Results of BV photometry 1969-70 (Uppsala refractor)". Private Communication. Bibcode: 1970Priv.........0H. 
  7. ↑ 7.0 7.1 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. doi:10.1134/S1063773706110065. ISSN 1063-7737. Bibcode: 2006AstL...32..759G. 
  8. ↑ Griffin, R. F. (August 2012). "Spectroscopic binary orbits from photoelectric radial velocities - Paper 225: HR 1313, HR 3567, HR 3907, and HR 6239; with a note on delta Boo, HD 146815, 64 Aql, and 75 Dra". The Observatory 132 (4): 234–252. ISSN 0029-7704. Bibcode: 2012Obs...132..234G. 
  9. ↑ 9.0 9.1 9.2 9.3 Dotter, Aaron; Chaboyer, Brian; Jevremović, Darko; Kostov, Veselin; Baron, E.; Ferguson, Jason W. (September 2008). "The Dartmouth Stellar Evolution Database". The Astrophysical Journal Supplement Series 178 (1): 89–101. doi:10.1086/589654. ISSN 0067-0049. Bibcode: 2008ApJS..178...89D. 
  10. ↑ Kervella, P.; Thévenin, F.; Di Folco, E.; Ségransan, D. (October 2004). "The angular sizes of dwarf stars and subgiants". Astronomy & Astrophysics 426 (1): 297–307. doi:10.1051/0004-6361:20035930. ISSN 0004-6361. Bibcode: 2004A&A...426..297K. 
  11. ↑ 11.0 11.1 11.2 11.3 11.4 Feuillet, Diane K.; Bovy, Jo; Holtzman, Jon; Girardi, Léo; MacDonald, Nick; Majewski, Steven R.; Nidever, David L. (20 January 2016). "Determining Ages of APOGEE Giants with Known Distances". The Astrophysical Journal 817 (1): 40. doi:10.3847/0004-637X/817/1/40. Bibcode: 2016ApJ...817...40F. 
  12. ↑ 12.0 12.1 12.2 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. doi:10.1086/342613. ISSN 0004-637X. Bibcode: 2002ApJ...578..943D. 
  13. ↑ "HD 26755". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=HD+26755. 
  14. ↑ Eggleton, P. P.; Tokovinin, A. A. (11 September 2008). "A catalogue of multiplicity among bright stellar systems". Monthly Notices of the Royal Astronomical Society 389 (2): 869–879. doi:10.1111/j.1365-2966.2008.13596.x. ISSN 0035-8711. Bibcode: 2008MNRAS.389..869E. 
  15. ↑ 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. doi:10.1093/mnras/stx2219. ISSN 0035-8711. Bibcode: 2017MNRAS.472.3805G. 



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