Astronomy:26 Boötis
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Boötes |
| Right ascension | 14h 32m 32.5423s[1] |
| Declination | +22° 15′ 36.2044″[1] |
| Apparent magnitude (V) | 5.91[2] |
| Characteristics | |
| Spectral type | F2 IV[3] |
| B−V color 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 ± 0.0774[1] mas |
| Distance | 188.2 ± 0.8 ly (57.7 ± 0.3 pc) |
| 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 (log g) | 3.93[5] cgs |
| Temperature | 6,826+40.5 −88.5[1] K |
| Metallicity [Fe/H] | 0.08[3] dex |
| Rotational velocity (v sin i) | 55.8±2.8[4] km/s |
| Age | 1.557[5] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
26 Boötis is a single[7] star in the northern constellation of Boötes,[6] located 188 light years away from the Sun.[1] It is visible to the naked eye as a dim, yellow-white hued star with an apparent visual magnitude of 5.91.[2] This object is moving closer to the Earth with a heliocentric radial velocity of −16.5 km/s.[2]
This is an F-type subgiant star with a stellar classification of F2 IV,[3] which suggests it has exhausted the supply of hydrogen at its core and is in the process of evolving into a giant. It is an estimated 1.6[5] billion years old with 1.46[5] times the mass of the Sun and 2.43[1] times the Sun's radius. The star is radiating 11.6[1] times the Sun's luminosity from its photosphere at an effective temperature of 6,826 K.[1] The rotation rate is moderately high, with a projected rotational velocity of 56 km/s.[4] 26 Boötis is a known source of radio emission.[8]
References
- ↑ 1.00 1.01 1.02 1.03 1.04 1.05 1.06 1.07 1.08 1.09 1.10 1.11 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G. Gaia DR2 record for this source at VizieR.
- ↑ 2.0 2.1 2.2 2.3 2.4 Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters 38 (5): 331, doi:10.1134/S1063773712050015, Bibcode: 2012AstL...38..331A.
- ↑ 3.0 3.1 3.2 Balachandran, Suchitra (May 1, 1990), "Lithium depletion and rotation in main-sequence stars", Astrophysical Journal, Part 1 354: 310–332, doi:10.1086/168691, Bibcode: 1990ApJ...354..310B.
- ↑ 4.0 4.1 4.2 Ammler-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, doi:10.1051/0004-6361/201118724, Bibcode: 2012A&A...542A.116A.
- ↑ 5.0 5.1 5.2 5.3 5.4 David, 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, doi:10.1088/0004-637X/804/2/146, Bibcode: 2015ApJ...804..146D.
- ↑ 6.0 6.1 "26 Boo". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=26+Boo.
- ↑ 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, doi:10.1111/j.1365-2966.2008.13596.x, Bibcode: 2008MNRAS.389..869E.
- ↑ 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, doi:10.1051/0004-6361:20011831, Bibcode: 2002A&A...383.1062H.
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