HR 5110
| Observation data EpochJ2000EquinoxJ2000 | |
|---|---|
| Constellation | Canes Venatici |
| Right ascension | 13h34m47.80827s[2] |
| Declination | +37° 10′ 56.6979″[2] |
| Apparent magnitude(V) | 4.91[3] |
| Characteristics | |
| Spectral type | kA6hF1mF2[4](F2 IV + K0 IV)[5] |
| B−Vcolor index | 0.404±0.010[3] |
| Variable type | RS CVn[5] |
| Astrometry | |
| Radial velocity(Rv) | 6.43±0.24[3]km/s |
| Proper motion(μ) | RA:+84.63[2]mas/yr Dec.:−9.34[2]mas/yr |
| Parallax(π) | 21.90 ± 0.23mas[2] |
| Distance | 149 ± 2ly (45.7 ± 0.5pc) |
| Absolute magnitude(MV) | 1.61[3] |
| Orbit[6] | |
| 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° |
| Periastronepoch(T) | 2,445,766.655 |
| Details | |
| BH CVn A | |
| Mass | 1.5[6]M☉ |
| Radius | 2.6[6]R☉ |
| Luminosity | 19.01[3]L☉ |
| Surface gravity(logg) | 3.61±0.14[7]cgs |
| Temperature | 6,569±223[7]K |
| Metallicity[Fe/H] | −0.20[3]dex |
| Age | 1.36[7]Gyr |
| BH CVn B | |
| Mass | 0.8[6]M☉ |
| Radius | 3.4[6]R☉ |
| Other designations | |
| Database references | |
| SIMBAD | data |
HR 5110,also known asBH Canum Venaticorum,is abinary star[6]system in thenorthernconstellationofCanes Venatici.It is visible to the naked eye with anapparent visual magnitudeof 4.91.[3]Based upon an annualparallax shiftof21.90±0.23mas,[2]it is located 149light-yearsaway. The system is moving further from theSunwith a heliocentricradial velocityof 6.4 km/s.[3]
This is a close binary system with an orbital period of 2.6 days and an orbital plane that is oriented nearly face-on.[6]It may be considered anAlgol-typesemidetached binary.The hotter primary component has astellar classificationof F2 IV,[5]indicating it is anevolvingsubgiant starthat is leaving themain sequenceafter consuming the hydrogen at its core.
HR 5110 is classified as aRS Canum Venaticorum variablesystem, primarily due tochromospheric activityin the secondary component.[5]This star has a classification of K0 IV, matching aK-typesubgiantstar.[5]Based upon the close separation of the pair and the class of the secondary component, that latter is probably filling itsroche 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 polarstarspot.[6]
References
[edit]- ^"MAST: Barbara A. Mikulski Archive for Space Telescopes".Space Telescope Science Institute.Retrieved8 December2021.
- ^abcdefvan 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,S2CID18759600.
- ^abcdefghAnderson, 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,S2CID119257644.
- ^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,S2CID122811461.
- ^abcdeRansom, 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,S2CID18203880.
- ^abcdefghAbbuhl, 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,S2CID118373672,33
- ^abcDavid, 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,S2CID33401607.
- ^"V* BH CVn".SIMBAD.Centre de données astronomiques de Strasbourg.Retrieved2018-06-07.
