Astronomy:HD 26755

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Short description: Binary star system in Camelopardalis
HD 26755
Camelopardalis constellation map.svg
Red circle.svg
Location of HD 26755 on the map (circled)
Observation data
Epoch J2000.0   Equinox (celestial coordinates)
Constellation Camelopardalis
Right ascension  04h 17m 08.09353s[1]
Declination +57° 51′ 37.1513″[1]
Apparent magnitude (V) 5.72±0.01[2]
Characteristics
Spectral type K1 III[3]
B−V color index +1.09[4]
Astrometry
Radial velocity (Rv)−38.2±1.6[5] km/s
Proper motion (μ) RA: +29.108[1] mas/yr
Dec.: −25.942[1] mas/yr
Parallax (π)12.0207 ± 0.1939[1] mas
Distance271 ± 4 ly
(83 ± 1 pc)
Absolute magnitude (MV)+1.21[6]
Orbit[7]
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[8] M☉
Radius9.44±0.47[9] R☉
Luminosity42.5±1.3[1] L☉
Surface gravity (log g)2.58±0.11[10] cgs
Temperature4,717±92[10] K
Metallicity [Fe/H]+0.17±0.05[10] dex
Rotational velocity (v sin i)1±1[11] km/s
Age2.13[8] Gyr
Other designations
BD+57°787, GC 5139, HD 26755, HIP 19983, HR 1313, SAO 24514[12]
Database references
SIMBADdata

HD 26755, also known as HR 1313, is a spectroscopic binary[11][13] located in the northern circumpolar constellation Camelopardalis, the giraffe. It has an apparent magnitude of 5.72,[2] 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[1] and is currently drifitng closer with a heliocentric radial velocity of −38 km/s.[5] At its current distance, HD 26755's brightness is diminished by 0.19 magnitudes due to interstellar dust.[14]

The visible component is an evolved red giant with a stellar classification of K1 III.[3] It is estimated to be 2.13 billion years old,[8] 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[8] and radiates 42.5 times the luminosity of the Sun[1] from its enlarged photosphere at an effective temperature of 4,717 K,[10] 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.[10] It spins slowly with a projected rotational velocity of 1 km/s,[11] which is poorly constrained.

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 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.
  2. ↑ 2.0 2.1 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. 
  3. ↑ 3.0 3.1 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. 
  4. ↑ Haggkvist, L.; Oja, T. (1970). "Results of BV photometry 1969-70 (Uppsala refractor)". Private Communication. Bibcode: 1970Priv.........0H. 
  5. ↑ 5.0 5.1 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. 
  6. ↑ Anderson, E.; Francis, Ch. (May 2012). "XHIP: An extended hipparcos compilation". Astronomy Letters 38 (5): 331–346. doi:10.1134/S1063773712050015. ISSN 1063-7737. Bibcode: 2012AstL...38..331A. 
  7. ↑ 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. 
  8. ↑ 8.0 8.1 8.2 8.3 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. 
  9. ↑ 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. 
  10. ↑ 10.0 10.1 10.2 10.3 10.4 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. 
  11. ↑ 11.0 11.1 11.2 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. 
  12. ↑ "HD 26755". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=HD+26755. 
  13. ↑ 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. 
  14. ↑ 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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