26 Boötis

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26 Boötis
Observation data
Epoch J2000      Equinox J2000
Constellation Boötes
Right ascension  14h 32m 32.5423s[1]
Declination +22° 15′ 36.2044″[1]
Apparent magnitude (V) 5.91[2]
Spectral type F2 IV[3]
B−V color index 0.391±0.005[2]
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
Distance188.2 ± 0.8 ly
(57.7 ± 0.3 pc)
Absolute magnitude (MV)2.20[4]
Mass1.46[5] M
[1] R
Luminosity11.553±0.065[1] L
Surface gravity (log g)3.93[5] cgs
[1] K
Metallicity [Fe/H]0.08[3] dex
Rotational velocity (v sin i)55.8±2.8[4] km/s
Age1.557[5] Gyr
Other designations
26 Boo, BD+22°2715, FK5 3151, GC 19611, HD 127739, HIP 71115, HR 5434, SAO 83395[6]
Database references

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]


  1. ^ a b c d e f g h i j k l Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data 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 source at VizieR.
  2. ^ a b c d e 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.
  3. ^ a b c Balachandran, 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.
  4. ^ a b c Ammler-von Eiff, M.; Reiners, A. (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.
  5. ^ a b c d e 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, arXiv:1501.03154, Bibcode:2015ApJ...804..146D, doi:10.1088/0004-637X/804/2/146.
  6. ^ a b "26 Boo". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved May 10, 2019.
  7. ^ 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.
  8. ^ Hui, H.; Rui, W. (March 2002), "Optical positions of 55 radio stars from astrolabe observations from the Yunnan Observatory", Astronomy and Astrophysics, 383: 1062–1066, Bibcode:2002A&A...383.1062H, doi:10.1051/0004-6361:20011831.