14 Boötis

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14 Boötis
Observation data
Epoch J2000      Equinox
Constellation Boötes
Right ascension  14h 14m 05.17971s[1]
Declination +12° 57′ 33.9997″[1]
Apparent magnitude (V) 5.53[2]
Characteristics
Spectral type F8 V[3]
B−V color index 0.55[2]
Astrometry
Radial velocity (Rv) −39.6±0.1[4] km/s
Proper motion (μ) RA: −253.97[1] mas/yr
Dec.: −54.47[1] mas/yr
Parallax (π) 29.7478 ± 0.1000[1] mas
Distance 109.6 ± 0.4 ly
(33.6 ± 0.1 pc)
Absolute magnitude (MV) 2.92[5]
Details
14 Boötis A
Mass 1.46[4] M
Radius 2.12+0.06
−0.03
[1] R
Luminosity 5.879+0.024
−0.026
[1] L
Surface gravity (log g) 3.85±0.10[6] cgs
Temperature 6,169+53
−81
[1] K
Metallicity [Fe/H] 0.07±0.10[6] dex
Rotation 26[6]
Rotational velocity (v sin i) 5.6[7] km/s
Age 2.60[4] Gyr
Other designations
14 Boo, BD+13°2764, HD 124570, HIP 69536, HR 5323, SAO 100925, WDS J14141+1258AB, LTT 14163[8]
Database references
SIMBAD data

14 Boötis is a possible binary star[9] system located 110 light years away from the Sun in the northern constellation of Boötes. It is visible to the naked eye as a dim, yellow-white hued star with a combined apparent visual magnitude of 5.53.[2] This system is moving closer to the Earth with a heliocentric radial velocity of −40 km/s.[4] It has a relatively high proper motion, traversing the celestial sphere at the rate of 0.260 arc seconds per annum.[10]

The component of this system remain unresolved as of 2002;[11] Eggleton and Tokovinin (2008) listed an angular separation of 0.2.[9] The visible component is an F-type main-sequence star with a stellar classification of F8 V[3] There are enhanced barium lines in the star's spectrum, but these are likely caused by regions of photospheric activity rather than being a barium star.[12] It is 2.6[4] billion years old and is spinning with a projected rotational velocity of 5.6 km/s,[7] giving it a rotation period of 26 days.[6]

14 Boötis has 1.46[4] times the mass of the Sun and 2.1[1] times the Sun's radius. It is radiating 5.9[1] times the luminosity of the Sun from its photosphere at an effective temperature of 6,169 K.[1] The metallicity is near solar, based on the abundance of iron in the stellar atmosphere.[6]

References[edit]

  1. ^ a b c d e f g h i j k 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 Takeda, Yoichi; et al. (February 2005), "High-Dispersion Spectra Collection of Nearby F--K Stars at Okayama Astrophysical Observatory: A Basis for Spectroscopic Abundance Standards", Publications of the Astronomical Society of Japan, 57 (1): 13–25, Bibcode:2005PASJ...57...13T, doi:10.1093/pasj/57.1.13.
  3. ^ a b Abt, Helmut A. (2009), "MK Classifications of Spectroscopic Binaries", The Astrophysical Journal Supplement, 180 (1): 117–18, Bibcode:2009ApJS..180..117A, doi:10.1088/0067-0049/180/1/117.
  4. ^ a b c d e f Casagrande, L.; et al. (June 2011), "New constraints on the chemical evolution of the solar neighbourhood and Galactic disc(s). Improved astrophysical parameters for the Geneva-Copenhagen Survey", Astronomy and Astrophysics, 530: A138, arXiv:1103.4651, Bibcode:2011A&A...530A.138C, doi:10.1051/0004-6361/201016276.
  5. ^ Takeda, Yoichi (April 2007), "Fundamental Parameters and Elemental Abundances of 160 F-G-K Stars Based on OAO Spectrum Database", Publications of the Astronomical Society of Japan, 59 (2): 335–356, Bibcode:2007PASJ...59..335T, doi:10.1093/pasj/59.2.335.
  6. ^ a b c d e Reinhold, Timo; et al. (January 2019), "Transition from spot to faculae domination. An alternate explanation for the dearth of intermediate Kepler rotation periods", Astronomy & Astrophysics, 621: 14, arXiv:1810.11250, Bibcode:2019A&A...621A..21R, doi:10.1051/0004-6361/201833754, A21.
  7. ^ a b Pizzolato, N.; Maggio, A.; Sciortino, S. (September 2000), "Evolution of X-ray activity of 1-3 Msun late-type stars in early post-main-sequence phases", Astronomy and Astrophysics, 361: 614–628, Bibcode:2000A&A...361..614P
  8. ^ "14 Boo". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-01-26.
  9. ^ a b 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.
  10. ^ Lépine, Sébastien; Shara, Michael M. (March 2005), "A Catalog of Northern Stars with Annual Proper Motions Larger than 0.15" (LSPM-NORTH Catalog)", The Astronomical Journal, 129 (3): 1483–1522, arXiv:astro-ph/0412070, Bibcode:2005AJ....129.1483L, doi:10.1086/427854.
  11. ^ Roberts, Lewis C., Jr. (May 2011), "Astrometric and photometric measurements of binary stars with adaptive optics: observations from 2002", Monthly Notices of the Royal Astronomical Society, 413 (2): 1200–1205, arXiv:1012.3383, Bibcode:2011MNRAS.413.1200R, doi:10.1111/j.1365-2966.2011.18205.x.
  12. ^ Pakhomov, Yu. V. (May 2018), "Spectroscopic analysis of barium dwarfs", in Bisikalo, D. V.; Wiebe, D. S. (eds.), Proceedings of the 2018 acad. A.A. Boyarchuk Memorial Conference, INASAN Science Proceedings, Moscow: Yanus-K, pp. 23–28, Bibcode:2018abmc.conf...23P, doi:10.26087/INASAN.2018.1.1.004.

External links[edit]