26 Boötis
| Observation data EpochJ2000EquinoxJ2000 | |
|---|---|
| Constellation | Boötes |
| Right ascension | 14h32m32.5423s[1] |
| Declination | +22° 15′ 36.2044″[1] |
| Apparent magnitude(V) | 5.91[2] |
| Characteristics | |
| Spectral type | F2 IV[3] |
| B−Vcolor index | 0.391±0.005[2] |
| Astrometry | |
| Radial velocity(Rv) | −16.5±1.8[2]km/s |
| Proper motion(μ) | RA:–127.019[1]mas/yr Dec.:+39.662[1]mas/yr |
| Parallax(π) | 17.3311 ± 0.0774mas[1] |
| Distance | 188.2 ± 0.8ly (57.7 ± 0.3pc) |
| Absolute magnitude(MV) | 2.20[4] |
| Details | |
| Mass | 1.46[5]M☉ |
| Radius | 2.43+0.03 −0.06[1]R☉ |
| Luminosity | 11.553±0.065[1]L☉ |
| Surface gravity(logg) | 3.93[5]cgs |
| Temperature | 6,826+40.5 −88.5[1]K |
| Metallicity[Fe/H] | 0.08[3]dex |
| Rotational velocity(vsini) | 55.8±2.8[4]km/s |
| Age | 1.557[5]Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
26 Boötisis a single[7]starin the northernconstellationofBoötes,[6]located 188light yearsaway from the Sun.[1]It is visible to the naked eye as a dim, yellow-white hued star with anapparent visual magnitudeof 5.91.[2]This object is moving closer to the Earth with a heliocentricradial velocityof −16.5 km/s.[2]
This is anF-typesubgiant starwith astellar classificationof F2 IV,[3]which suggests it has exhausted the supply of hydrogen at itscoreand is in the process ofevolvinginto agiant.It is an estimated 1.6[5]billion years old with 1.46[5]times themass of the Sunand 2.43[1]times theSun's radius.The star is radiating 11.6[1]times theSun's luminosityfrom itsphotosphereat aneffective temperatureof 6,826 K.[1]The rotation rate is moderately high, with aprojected rotational velocityof 56 km/s.[4]26 Boötis is a known source of radio emission.[8]
References
[edit]- ^abcdefghijklBrown, A. G. A.;et al. (Gaia collaboration) (August 2018)."GaiaData Release 2: Summary of the contents and survey properties ".Astronomy & Astrophysics.616.A1.arXiv:1804.09365.Bibcode:2018A&A...616A...1G.doi:10.1051/0004-6361/201833051.Gaia DR2 record for this sourceatVizieR.
- ^abcdeAnderson, 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.
- ^abcBalachandran, Suchitra (May 1, 1990), "Lithium depletion and rotation in main-sequence stars",Astrophysical Journal, Part 1,354:310–332,Bibcode:1990ApJ...354..310B,doi:10.1086/168691.
- ^abcAmmler-von Eiff, Matthias; Reiners, Ansgar (June 2012), "New measurements of rotation and differential rotation in A-F stars: are there two populations of differentially rotating stars?",Astronomy & Astrophysics,542:A116,arXiv:1204.2459,Bibcode:2012A&A...542A.116A,doi:10.1051/0004-6361/201118724,S2CID53666672.
- ^abcdeDavid, 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.
- ^ab"26 Boo".SIMBAD.Centre de données astronomiques de Strasbourg.RetrievedMay 10,2019.
- ^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.
- ^Hui, H.; Rui, W. (March 2002), "Optical positions of 55 radio stars from astrolabe observations from the Yunnan Observatory",Astronomy and Astrophysics,383(3): 1062–1066,Bibcode:2002A&A...383.1062H,doi:10.1051/0004-6361:20011831.
