24 Boötis
| Observation data EpochJ2000EquinoxJ2000 | |
|---|---|
| Constellation | Boötes |
| Right ascension | 14h28m37.8130s[1] |
| Declination | +49° 50′ 41.461″[1] |
| Apparent magnitude(V) | +5.59[2] |
| Characteristics | |
| Spectral type | G4 III-IV Fe-1[3] |
| B−Vcolor index | 0.85±0.02[2] |
| Astrometry | |
| Radial velocity(Rv) | −8.116±0.024[2]km/s |
| Proper motion(μ) | RA:−304.035[1]mas/yr Dec.:-46.861[1]mas/yr |
| Parallax(π) | 10.00 ± 0.25mas[1] |
| Distance | 326 ± 8ly (100 ± 3pc) |
| Absolute magnitude(MV) | +0.59[2] |
| Details[2] | |
| Mass | 0.97±0.06M☉ |
| Radius | 12.24±1.16R☉ |
| Luminosity | 61.7+10.8 −9.2L☉ |
| Surface gravity(logg) | 2.17±0.02cgs |
| Temperature | 4,863±5K |
| Metallicity[Fe/H] | −0.77±0.01dex |
| Rotational velocity(vsini) | 2.57±0.73km/s |
| Age | 7.2+1.9 −1.5Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
24 Boötisorg Boötisis a single,[5]yellow-huedstarin theconstellationBoötes.It is faintly visible to the naked eye with anapparent visual magnitudeof +5.59.[2]Based upon an annualparallax shiftof 10.00mas,[1]it is located around 326light yearsfrom the Sun. The star is moving closer to the Sun with aradial velocityof −8 km/s.[2]It is athick diskstar with a high galacticspace velocityand anorbital eccentricityof0.47±0.01that carries it as close as3.30±0.05 kpcto theGalactic Center,and as far away as9.15±0.02 kpc.[6]Anextrasolar planetwas discovered orbiting this star in 2018.[7]
This is anevolvingred giant[6]star with astellar classificationofG4 III-IV Fe-1,[3]with the notation indicating thespectrumshows blended characteristics of asubgiantandgiant starwith an underabundance of iron. At the age of around 7 billion years old, it has 0.97 times themass of the Sunbut has expanded to 12 times theSun's radius.The star is radiating 61.7 times theSun's luminosityfrom its enlargedphotosphereat aneffective temperatureof 4,863 K.[2]
Planetary system
[edit]24 Boötis b was discovered by Takuya Takarada and collaborators using theDoppler Spectroscopymethod, during theOkayama Planet Searchradial velocity survey of G and K giants atOkayama Astrophysical Observatory.Thepreprintannouncing the discovery was published on thearXiveprintrepository on April 11, 2018[7]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | ≥0.91+0.13 −0.10MJ |
0.190+0.012 −0.009 |
30.3506+0.0078 −0.0077 |
0.042+0.048 −0.029 |
— | — |
References
[edit]- ^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.
- ^abcdefghNiedzielski, 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
- ^abKeenan, 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.
- ^"g Boo".SIMBAD.Centre de données astronomiques de Strasbourg.Retrieved2018-02-09.
- ^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,S2CID14878976.
- ^abPakhomov, 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,S2CID119161642.
- ^abcTakarada, 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.S2CID119027104.
