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26 Boötis

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Star in the constellation Boötes
26 Boötis
Observation data
Epoch J2000      Equinox J2000
Constellation Boötes
Right ascension 14 32 32.5423
Declination +22° 15′ 36.2044″
Apparent magnitude (V) 5.91
Characteristics
Spectral type F2 IV
B−V color index 0.391±0.005
Astrometry
Radial velocity (Rv)−16.5±1.8 km/s
Proper motion (μ) RA: –127.019 mas/yr
Dec.: +39.662 mas/yr
Parallax (π)17.3311 ± 0.0774 mas
Distance188.2 ± 0.8 ly
(57.7 ± 0.3 pc)
Absolute magnitude (MV)2.20
Details
Mass1.46 M
Radius2.43+0.03
−0.06 R
Luminosity11.553±0.065 L
Surface gravity (log g)3.93 cgs
Temperature6,826+40.5
−88.5 K
Metallicity 0.08 dex
Rotational velocity (v sin i)55.8±2.8 km/s
Age1.557 Gyr
Other designations
26 Boo, BD+22°2715, FK5 3151, GC 19611, HD 127739, HIP 71115, HR 5434, SAO 83395
Database references
SIMBADdata

26 Boötis is a single star in the northern constellation of Boötes, located 188 light years away from the Sun. It is visible to the naked eye as a dim, yellow-white hued star with an apparent visual magnitude of 5.91. This object is moving closer to the Earth with a heliocentric radial velocity of −16.5 km/s.

This is an F-type subgiant star with a stellar classification of F2 IV, 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 billion years old with 1.46 times the mass of the Sun and 2.43 times the Sun's radius. The star is radiating 11.6 times the Sun's luminosity from its photosphere at an effective temperature of 6,826 K. The rotation rate is moderately high, with a projected rotational velocity of 56 km/s. 26 Boötis is a known source of radio emission.

References

  1. ^ 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. ^ 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, S2CID 119257644.
  3. ^ 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. ^ 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, arXiv:1204.2459, Bibcode:2012A&A...542A.116A, doi:10.1051/0004-6361/201118724, S2CID 53666672.
  5. ^ 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, S2CID 33401607.
  6. ^ "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, S2CID 14878976.
  8. 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.
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