Star in the constellation Boötes
39 Boötis Observation dataEpoch J2000 Equinox J2000 Constellation Boötes Right ascension 14h 49m 41.29265s [ 1] Declination +48° 43′ 14.9077″[ 1] Apparent magnitude (V)5.68[ 2] (6.36 + 6.72) [ 3] Characteristics Spectral type F8V + F7V [ 4] Astrometry Radial velocity (Rv )± 0.3[ 5] km/s Proper motion (μ)RA: −77.94 [ 1] mas /yr Dec.: 100.83 [ 1] mas /yr Parallax (π)14.58± 0.51 mas [ 1] Distance 224 ± 8 ly pc ) Absolute magnitude (MV )2.53[ 6] Orbit [ 7] Period (P)12.822 d Eccentricity (e)0.39 Periastron epoch (T)JD Argument of periastron (ω)97.1° Semi-amplitude 1 )58.3 km/s Semi-amplitude (K2 )72.2 km/s Details 39 Boo A Mass 1.29/1.05[ 8] M ☉ Metallicity 0.06[ 9] dex Rotational velocity (v sin i )161.0[ 6] Age 1.30[ 9] Gyr 39 Boo B Mass 1.25[ 8] M ☉ Other designations 39 Boo AG +48°1158BD +49°2326HD 131041HIP 72524HR 5538SAO 45231CCDM J14497+4843WDS J14497+4843[ 10] Database references SIMBAD data
39 Boötis is atriple star [ 3] [ 1] light years away from the Sun in the northernconstellation ofBoötes .[ 10] apparent magnitude of 5.68.[ 2] radial velocity of −31 km/s.[ 5]
The magnitude 6.36[ 3] spectroscopic binary system with anorbital period of 12.822 days, aneccentricity of 0.39,[ 7] angular separation ofmas stellar classification of F8V,[ 4] F-type main-sequence star , with individual massed of 1.29 and 1.05[ 8] mass of the Sun . Component B is of magnitude 6.72[ 3] [ 4] [ 8] ″ [ 8] X-ray emission with aluminosity of× 1028 erg s−1 [ 11]
It was a transferred byJérôme Lalande fromBoötes toQuadrans Muralis .[ 12] International Astronomical Union officially recognised constellations, Quadrans Muralis becameobsolete , so this star was moved back to Boötes.
^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 .S2CID 18759600 . ^a b 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 ,S2CID 119257644 . ^a b c d Eggleton, P. P.; Tokovinin, A. A. (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 S2CID 14878976 . ^a b c 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 .S2CID 122811461 . ^a b Gontcharov, G. A. (2006). "Pulkovo Compilation of Radial Velocities for 35 495 Hipparcos stars in a common system".Astronomy Letters .32 (11):759– 771.arXiv :1606.08053 Bibcode :2006AstL...32..759G .doi :10.1134/S1063773706110065 .S2CID 119231169 . ^a b Pizzolato, N.; et al. (September 2000). "Evolution of X-ray activity of 1-3 Msun late-type stars in early post-main-sequence phases".Astronomy and Astrophysics .361 :614– 628.Bibcode :2000A&A...361..614P . ^a b Pourbaix, D.; et al. (2004). "SB9: The Ninth Catalogue of Spectroscopic Binary Orbits".Astronomy & Astrophysics .424 :727– 732.arXiv :astro-ph/0406573 Bibcode :2004A&A...424..727P .doi :10.1051/0004-6361:20041213 .S2CID 119387088 . ^a b c d e Tokovinin, A.; et al. (2008). "Tertiary companions to close spectroscopic binaries".Multiple Stars Across the H-R Diagram, ESO Astrophysics Symposia . Berlin Heidelberg. p. 129.arXiv :astro-ph/0601518 Bibcode :2006yCat..34500681T .doi :10.1051/0004-6361:20054427 .ISBN 978-3-540-74744-4 ^a b Casagrande, L.; et al. (June 2011). "New constraints on the chemical evolution of the solar neighbourhood and Galactic disc(s). Improved astrophysical parameters for the Geneva-Copenhagen Survey".Astronomy and Astrophysics .530 : A138.arXiv :1103.4651 Bibcode :2011A&A...530A.138C .doi :10.1051/0004-6361/201016276 .S2CID 56118016 . ^a b "39 Boo" .SIMBAD Centre de données astronomiques de Strasbourg . RetrievedMay 12, 2019 .^ Pizzolato, N.; et al. (September 2000). "Evolution of X-ray activity of 1-3 Msun late-type stars in early post-main-sequence phases".Astronomy and Astrophysics .361 :614– 628.Bibcode :2000A&A...361..614P . ^ Smyth, William Henry (1844).A Cycle of Celestial Objects: For the Use of Naval, Military, and Private Astronomers
