Astronomy:HD 36848

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Short description: Star in the constellation Columba
HD 36848
Observation data
Epoch J2000.0   Equinox (celestial coordinates)
Constellation Columba
Right ascension  05h 32m 51.4130s[1]
Declination −38° 30′ 48.1306″[1]
Apparent magnitude (V) 5.46±0.01[2]
Characteristics
Evolutionary stage red giant branch[3]
Spectral type K2/3 III[4]
B−V color index +1.22[5]
Astrometry
Radial velocity (Rv)−0.6±0.1[6] km/s
Proper motion (μ) RA: +48.475[1] mas/yr
Dec.: −10.959[1] mas/yr
Parallax (π)18.7844 ± 0.0462[1] mas
Distance173.6 ± 0.4 ly
(53.2 ± 0.1 pc)
Absolute magnitude (MV)+1.84[7]
Details
Mass1.18[8] M☉
Radius8.71+0.62−0.58[9] R☉
Luminosity24.54[10] L☉
Surface gravity (log g)2.7±0.2[11] cgs
Temperature4,460±70[11] K
Metallicity [Fe/H]+0.28±0.05[11] dex
Rotational velocity (v sin i)<2.7[12] km/s
Age7.33[8] Gyr
Other designations
CD−38°2085, CPD−38°653, GC 6889, HD 36848, HIP 25993, HR 1877, SAO 195948[13]
Database references
SIMBADdata

HD 36848 (HR 1877) is a star in the southern constellation Columba. It has an apparent magnitude of 5.46,[2] allowing it to be faintly seen with a naked eye. The star is relatively close at a distance of 174 light years[1] and is moving closer with a heliocentric radial velocity of only −0.6 km/s.[6]

HD 36848 has a stellar classification of K2/3 III — intermediate between a K2 and 3 giant star. It is on the red giant branch,[3] meaning it has exhausted its core hydrogen and is now fusing hydrogen in a shell outside the core. It has a comparable mass to the Sun[8] but has expanded to 8.71 times the radius of the Sun[9] after 7.33 billion years.[8] It shines with a luminosity of 24.5 solar luminosity[10] from its enlarged photosphere at an effective temperature of 4,460 K,[11] giving t an orange hue. The star is metal enriched with an iron abundance 90% greater than that of the Sun[11] and spins with a projected rotational velocity lower than 2.7 km/s.[12]

The star's multiplicity status isn't generally agreed on. Eggleton et al. classifies it as a solitary star[14] while De Mederios et al. finds it to be a probable spectroscopic binary.[12]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 Brown, A. G. A. (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics 649: A1. doi:10.1051/0004-6361/202039657. Bibcode: 2021A&A...649A...1G.  Gaia EDR3 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 Setiawan, J. et al. (July 2004). "Precise radial velocity measurements of G and K giants. Multiple systems and variability trend along the Red Giant Branch". Astronomy and Astrophysics 421: 241–254. doi:10.1051/0004-6361:20041042-1. Bibcode: 2004A&A...421..241S. 
  4. ↑ Houk, N. (1982). Michigan Catalogue of Two-dimensional Spectral Types for the HD stars. Volume_3. Declinations -40_ƒ0 to -26_ƒ0.. Bibcode: 1982mcts.book.....H. 
  5. ↑ Johnson, H. L.; Mitchell, R. I.; Iriarte, B.; Wisniewski, W. Z. (1966). "UBVRIJKL Photometry of the Bright Stars". Communications of the Lunar and Planetary Laboratory 4: 99–110. Bibcode: 1966CoLPL...4...99J. 
  6. ↑ 6.0 6.1 Jofré, E.; Petrucci, R.; Saffe, C.; Saker, L.; Artur de la Villarmois, E.; Chavero, C.; Gómez, M.; Mauas, P. J. D. (26 January 2015). "Stellar parameters and chemical abundances of 223 evolved stars with and without planets". Astronomy & Astrophysics 574: A50. doi:10.1051/0004-6361/201424474. ISSN 0004-6361. Bibcode: 2015A&A...574A..50J. 
  7. ↑ Anderson, E.; Francis, Ch. (May 2012). "XHIP: An extended hipparcos compilation" (in en). Astronomy Letters 38 (5): 331–346. doi:10.1134/S1063773712050015. ISSN 1063-7737. Bibcode: 2012AstL...38..331A. 
  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. ↑ 9.0 9.1 Allende Prieto, C.; Lambert, D. L. (December 1999). "Fundamental parameters of nearby stars from the comparison with evolutionary calculations: masses, radii and effective temperatures". Astronomy and Astrophysics 352: 555–562. ISSN 0004-6361. Bibcode: 1999A&A...352..555A. 
  10. ↑ 10.0 10.1 Luck, R. Earle (25 August 2015). "Abundances in the Local Region. I. G and K Giants". The Astronomical Journal 150 (3): 88. doi:10.1088/0004-6256/150/3/88. ISSN 0004-6256. Bibcode: 2015AJ....150...88L. 
  11. ↑ 11.0 11.1 11.2 11.3 11.4 da Silva, L.; Girardi, L.; Pasquini, L.; Setiawan, J.; von der Lühe, O.; de Medeiros, J. R.; Hatzes, A.; Döllinger, M. P. et al. (12 September 2006). "Basic physical parameters of a selected sample of evolved stars". Astronomy & Astrophysics 458 (2): 609–623. doi:10.1051/0004-6361:20065105. ISSN 0004-6361. Bibcode: 2006A&A...458..609D. 
  12. ↑ 12.0 12.1 12.2 De Medeiros, J. R.; Alves, S.; Udry, S.; Andersen, J.; Nordström, B.; Mayor, M. (January 2014). "A catalog of rotational and radial velocities for evolved stars: V. Southern stars⋆⋆⋆". Astronomy & Astrophysics 561: A126. doi:10.1051/0004-6361/201220762. ISSN 0004-6361. Bibcode: 2014A&A...561A.126D. 
  13. ↑ "HR 1877". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=HR+1877. 
  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. 
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