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 mas[1] |
| 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 | |
| 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]- ^ 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.
- ^ 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.
- ^ 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, S2CID 122811461.
- ^ 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, S2CID 56118016.
- ^ 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.
- ^ 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, S2CID 119505516, A21.
- ^ 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.
- ^ "14 Boo". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-01-26.
- ^ 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, S2CID 14878976.
- ^ 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, S2CID 2603568.
- ^ 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, S2CID 118398949.
- ^ 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 (in Russian), Moscow: Yanus-K, pp. 23–28, Bibcode:2018abmc.conf...23P, doi:10.26087/INASAN.2018.1.1.004.
External links
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