Star in the constellation Boötes
24 Boötis or g Boötis is a single,[ 6] star in the constellation Boötes . It is faintly visible to the naked eye with an apparent visual magnitude of +5.59.[ 2] parallax shift of 10.59 mas ,[ 1] light years from the Sun. The star is moving closer to the Sun with a radial velocity of −8 km/s.[ 2] thick disk star with a high galactic space velocity and an orbital eccentricity of ± 0.01± 0.05 kpcGalactic Center , and as far away as ± 0.02 kpc[ 7] extrasolar planet was discovered orbiting this star in 2018.[ 8]
This is an evolving red giant [ 7] stellar classification of G4 III-IV Fe-1 ,[ 3] spectrum shows blended characteristics of a subgiant and giant star with an underabundance of iron. It has 1.46 times the mass of the Sun but has expanded to ten times the Sun's radius . The star is radiating 55 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,959 K.[ 4]
Planetary system
24 Boötis b was discovered by Takuya Takarada and collaborators using the Doppler Spectroscopy method, during the Okayama Planet Search radial velocity survey of G and K giants at Okayama Astrophysical Observatory . The preprint announcing the discovery was published on the arXiv eprint repository on April 11, 2018.[ 8]
References
^ a b c d e Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties" . Astronomy and Astrophysics . 674 : A1. arXiv :2208.00211 Bibcode :2023A&A...674A...1G . doi :10.1051/0004-6361/202243940 S2CID 244398875 . Gaia DR3 record for this source at VizieR .^ a b c d e f g Niedzielski, A.; et al. (January 2016), "The Penn State - Toruń Centre for Astronomy Planet Search stars", Astronomy & Astrophysics , 585 : 14, arXiv :1407.4956 Bibcode :2016A&A...585A..73N , doi :10.1051/0004-6361/201527362 , A73 ^ a b Keenan, Philip C.; McNeil, Raymond C. (1989), "The Perkins catalog of revised MK types for the cooler stars", Astrophysical Journal Supplement Series , 71 : 245, Bibcode :1989ApJS...71..245K , doi :10.1086/191373 . ^ a b Karovicova, I.; White, T. R.; Nordlander, T.; Casagrande, L.; Ireland, M.; Huber, D.; Jofré, P. (2020-08-01). "Fundamental stellar parameters of benchmark stars from CHARA interferometry - I. Metal-poor stars" . Astronomy & Astrophysics . 640 : A25. arXiv :2006.05411 Bibcode :2020A&A...640A..25K . doi :10.1051/0004-6361/202037590 . ISSN 0004-6361 . ^ "g Boo" . SIMBAD Centre de données astronomiques de Strasbourg . Retrieved 2018-02-09 .^ 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 Pakhomov, Yu. V. (February 2012), "Chemical composition of the atmospheres of red giants with high space velocities", Astronomy Letters , 38 (2): 101−116, arXiv :1312.3195 Bibcode :2012AstL...38..101P , doi :10.1134/S1063773712020053 , S2CID 119161642 . ^ a b c Takarada, Takuya; et al. (2018). "Planets around the evolved stars 24 Booties and γ Libra: A 30d-period planet and a double giant-planet system in possible 7:3 MMR". Publications of the Astronomical Society of Japan . 70 (4). arXiv :1804.04008 doi :10.1093/pasj/psy052 . S2CID 119027104 .
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