HR 5110

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HR 1550
Observation data
Epoch J2000      Equinox J2000
Constellation Canes Venatici
Right ascension  13h 34m 47.80827s[1]
Declination +37° 10′ 56.6979″[1]
Apparent magnitude (V) 4.91[2]
Spectral type kA6hF1mF2[3] (F2 IV + K0 IV)[4]
B−V color index 0.404±0.010[2]
Variable type RS CVn[4]
Radial velocity (Rv)6.43±0.24[2] km/s
Proper motion (μ) RA: +84.63[1] mas/yr
Dec.: −9.34[1] mas/yr
Parallax (π)21.90 ± 0.23[1] mas
Distance149 ± 2 ly
(45.7 ± 0.5 pc)
Absolute magnitude (MV)1.61[2]
Period (P)2.613214 d
Semi-major axis (a)0.017 AU
Eccentricity (e)0.00
Inclination (i)171.1°
Longitude of the node (Ω)89±10°
Periastron epoch (T)2445766.655
Mass1.5[5] M
Radius2.6[5] R
Luminosity19.01[2] L
Surface gravity (log g)3.61±0.14[6] cgs
Temperature6,569±223[6] K
Metallicity [Fe/H]−0.20[2] dex
Age1.36[6] Gyr
Mass0.8[5] M
Radius3.4[5] R
Other designations
BH CVn, BD+37° 2426, FK5 502, HD 118216, HIP 66257, HR 5110, SAO 63623[7]
Database references

HR 5110, also known as BH Canum Venaticorum, is a binary star[5] system in the northern constellation of Canes Venatici. It is visible to the naked eye with an apparent visual magnitude of 4.91.[2] Based upon an annual parallax shift of 21.90±0.23 mas,[1] it is located 149 light years away. The system is moving further from the Sun with a heliocentric radial velocity of 6.4 km/s.[2]

This is a close binary system with an orbital period of 2.6 days and an orbital plane that is oriented nearly face-on.[5] It may be considered an Algol-type semidetached binary. The hotter primary component has a stellar classification of F2 IV,[4] indicating it is an evolving subgiant star that is leaving the main sequence after consuming the hydrogen at its core.

HR 5110 is classified as a RS Canum Venaticorum variable system, primarily due to chromospheric activity in the secondary component.[4] This star has a classification of K0 IV, matching a K-type subgiant star.[4] Based upon the close separation of the pair and the class of the secondary component, that latter is probably filling its roche lobe. This star is most likely the source of the radio emission from this system, and the alignment of this signal is consistent with a polar star spot.[5]


  1. ^ a b c d e f van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357.
  2. ^ a b c d e f g h Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv:1108.4971, Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015.
  3. ^ Abt, Helmut A. (2009), "MK Classifications of Spectroscopic Binaries", The Astrophysical Journal Supplement, 180 (1): 117–18, Bibcode:2009ApJS..180..117A, doi:10.1088/0067-0049/180/1/117.
  4. ^ a b c d e Ransom, R. R.; et al. (April 2003), "Very Long Baseline Interferometry Imaging of the RS Canum Venaticorum Binary Star System HR 5110", The Astrophysical Journal, 587 (1): 390–397, arXiv:astro-ph/0301413, Bibcode:2003ApJ...587..390R, doi:10.1086/368070.
  5. ^ a b c d e f g h Abbuhl, E.; Mutel, R. L.; Lynch, C.; Güedel, M. (September 2015), "Radio Astrometry of the Close Active Binary HR5110", The Astrophysical Journal, 811 (1): 8, arXiv:1508.06654, Bibcode:2015ApJ...811...33A, doi:10.1088/0004-637X/811/1/33, 33
  6. ^ a b c David, Trevor J.; Hillenbrand, Lynne A. (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.
  7. ^ "V* BH CVn". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-06-07.