HD 36187

Last updated
HD 36187
Columba constellation map.svg
Red circle.svg
Location of HD 36187 (circled)
Observation data
Epoch J2000.0        Equinox J2000.0 (ICRS)
Constellation Columba
Right ascension 05h 28m 15.33500s [1]
Declination −37° 13′ 50.7477″ [1]
Apparent magnitude  (V)5.55±0.01 [2]
Characteristics
Evolutionary stage main sequence star [3]
Spectral type A1 V [4] [5]
B−V color index +0.02 [6]
Astrometry
Radial velocity (Rv)50±2 [7]  km/s
Proper motion (μ)RA: +10.887  mas/yr [1]
Dec.: +68.709  mas/yr [1]
Parallax (π)11.5707 ± 0.0576  mas [1]
Distance 282 ± 1  ly
(86.4 ± 0.4  pc)
Absolute magnitude  (MV)+0.84 [8]
Details
Mass 2.3+0.15
−0.12 [9]   M☉
Radius 2.43±0.12 [10]   R☉
Luminosity 48±2 [3]   L☉
Surface gravity (log g)4.10±0.14 [9]   cgs
Temperature 9,513±21 [11]   K
Metallicity [Fe/H]−0.16 [12]   dex
Rotational velocity (v sin i)145 [13]  km/s
Age 311+83
−149 [9]   Myr
Other designations
20 G. Columbae [14] , CD−37°2220, CPD−37°692, GC  6774, HD  36187, HIP  25608, HR  1835, SAO  195887 [15]
Database references
SIMBAD data

HD 36187, also known as HR 1835, is a solitary, [16] bluish-white hued star located in the southern constellation Columba, the dove. It has an apparent magnitude of 5.55, [2] making it faintly visible to the naked eye under ideal conditions. Based on parallax measurements from the Gaia spacecraft, it is estimated to be 282 light years away from the Solar System. [1] However, it is receding rapidly with a heliocentric radial velocity of 50  km/s . [7] At its current distance, HD 36187's brightness is diminished by 0.21 magnitude due to interstellar dust. [17]

HD 36187 has a stellar classification of either A1 V [4] [5] or A0 V, [18] depending on the source. Nevertheless, both classes indicate that it is an ordinary A-type main-sequence star that is fusing hydrogen in its core. It has double the mass [9] and radius of the Sun. [10] It radiates 48 times the luminosity of the Sun [3] from its photosphere at an effective temperature of 9,512  K . [11] HD 36187 is estimated to be 311 million years old, [9] having completed 66.9% of its main sequence lifetime. [3] Like many hot stars HR 1835 spins rapidly, having a projected rotational velocity of 145  km/s . [13]

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References

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  2. 1 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.
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  6. ↑ 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.
  7. 1 2 Kharchenko, N.V.; Scholz, R.-D.; Piskunov, A.E.; Röser, S.; Schilbach, E. (November 2007). "Astrophysical supplements to the ASCC-2.5: Ia. Radial velocities of ~55000 stars and mean radial velocities of 516 Galactic open clusters and associations". Astronomische Nachrichten. 328 (9): 889–896. arXiv: 0705.0878 . Bibcode:2007AN....328..889K. doi:10.1002/asna.200710776. eISSN   1521-3994. ISSN   0004-6337. S2CID   119323941.
  8. ↑ 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.
  9. 1 2 3 4 5 David, Trevor J.; Hillenbrand, Lynne A. (12 May 2015). "The Ages of Early-type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets". The Astrophysical Journal. 804 (2): 146. arXiv: 1501.03154 . Bibcode:2015ApJ...804..146D. doi: 10.1088/0004-637X/804/2/146 . eISSN   1538-4357.
  10. 1 2 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. arXiv: astro-ph/0404180 . Bibcode:2004A&A...426..297K. doi: 10.1051/0004-6361:20035930 . eISSN   1432-0746. ISSN   0004-6361.
  11. 1 2 Paunzen, E.; Schnell, A.; Maitzen, H. M. (October 2006). "An empirical temperature calibration for the Δa photometric system II: The A-type and mid F-type stars". Astronomy & Astrophysics. 458 (1): 293–296. arXiv: astro-ph/0607567 . Bibcode:2006A&A...458..293P. doi: 10.1051/0004-6361:20064889 . eISSN   1432-0746. ISSN   0004-6361.
  12. ↑ 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 . ISSN   0004-6361.
  13. 1 2 Royer, F.; Gerbaldi, M.; Faraggiana, R.; Gómez, A. E. (January 2002). "Rotational velocities of A-type stars". Astronomy & Astrophysics. 381 (1): 105–121. arXiv: astro-ph/0110490 . Bibcode:2002A&A...381..105R. doi: 10.1051/0004-6361:20011422 . eISSN   1432-0746. ISSN   0004-6361.
  14. ↑ Gould, Benjamin Apthorp (1878). "Uranometria Argentina : brillantez y posicion de las estrellas fijas, hasta la septima magnitud, comprendidas dentro de cien grados del polo austral : con atlas". Resultados del Observatorio Nacional Argentino. 1. Bibcode:1879RNAO....1.....G.
  15. ↑ "HD 36187". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved December 5, 2022.
  16. ↑ 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. arXiv: 0806.2878 . Bibcode:2008MNRAS.389..869E. doi: 10.1111/j.1365-2966.2008.13596.x . eISSN   1365-2966. ISSN   0035-8711.
  17. ↑ 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.
  18. ↑ Houk, N. (1982). Michigan Catalogue of Two-dimensional Spectral Types for the HD stars. Volume III: Declinations −40° to −26°. Bibcode:1982mcts.book.....H.
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