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.