20 Boötis

20 Boötis
Observation data; Epoch J2000 Equinox J2000
Constellation	Boötes
Right ascension	14h 19m 45.23505s
Declination	+16° 18′ 24.9955″
Apparent magnitude (V)	4.84
Characteristics
Spectral type	K3 III
B−V color index	1.228±0.001
Astrometry
Radial velocity (Rv)	−8.25±0.43 km/s
Proper motion (μ)	RA: –141.521 mas/yr ; Dec.: +60.274 mas/yr
Parallax (π)	17.8379 ± 0.1894 mas
Distance	183 ± 2 ly ; (56.1 ± 0.6 pc)
Absolute magnitude (MV)	1.01±0.09
Details
Mass	1.14±0.19 M☉
Radius	12.18+0.26; −0.36 R☉
Luminosity	51.99±0.66 L☉
Surface gravity (log g)	2.36±0.08 cgs
Temperature	4,472 K
Metallicity [Fe/H]	0.16 dex
Rotation	848 days
Rotational velocity (v sin i)	1.0 km/s
Age	5.21±2.28 Gyr
Other designations
	20 Boo, NSV 6631, BD+16°2637, FK5 3135, GC 19334, GJ 3841, HD 125560, HIP 70027, HR 5370, SAO 100980
Database references
SIMBAD	data

20 Boötis is a single^[7] star in the northern constellation of Boötes, located 183 light years away from the Sun. It is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of 4.84.^[2] The star has a relatively high proper motion, traversing the celestial sphere at the rate of 0.154 arc seconds per annum.^[8] It is moving closer to the Earth with a heliocentric radial velocity of −8 km/s.^[2]

This is an aging K-type giant star with a stellar classification of K3 III.^[3] It is a red clump giant,^[9] which indicates it is on the horizontal branch and is generating energy through helium fusion at its core. The star is around five billion years old with 1.1^[4] times the mass of the Sun and has expanded to 12^[1] times the Sun's radius. It is radiating 52^[1] times the luminosity of the Sun from its swollen photosphere at an effective temperature of 4,472 K.^[4]

References

^ ^a ^b ^c ^d ^e ^f ^g ^h ⁱ 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 ^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, S2CID 119257644.
^ ^a ^b Roman, Nancy G. (July 1952), "The Spectra of the Bright Stars of Types F5-K5", Astrophysical Journal, 116: 122, Bibcode:1952ApJ...116..122R, doi:10.1086/145598.
^ ^a ^b ^c ^d da Silva, L.; et al. (November 2006), "Basic physical parameters of a selected sample of evolved stars", Astronomy and Astrophysics, 458 (2): 609–623, arXiv:astro-ph/0608160, Bibcode:2006A&A...458..609D, doi:10.1051/0004-6361:20065105, S2CID 9341088.
^ ^a ^b Setiawan, J.; et al. (July 2004), "Precise radial velocity measurements of G and K giants. Multiple systems and variability trend along the Red Giant Branch", Astronomy and Astrophysics, 421: 241–254, Bibcode:2004A&A...421..241S, doi:10.1051/0004-6361:20041042-1.
^ "20 Boo". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved May 8, 2019.
^ 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.
^ Alves, David R. (August 2000), "K-Band Calibration of the Red Clump Luminosity", The Astrophysical Journal, 539 (2): 732–741, arXiv:astro-ph/0003329, Bibcode:2000ApJ...539..732A, doi:10.1086/309278, S2CID 16673121

External links

[GaiaDR2-1] ^ ^a ^b ^c ^d ^e ^f ^g ^h ⁱ 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.

[Anderson2012-2] 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.

[Roman1952-3] Roman, Nancy G. (July 1952), "The Spectra of the Bright Stars of Types F5-K5", Astrophysical Journal, 116: 122, Bibcode:1952ApJ...116..122R, doi:10.1086/145598.

[aaa458_2_609-4] Silva, L.; et al. (November 2006), "Basic physical parameters of a selected sample of evolved stars", Astronomy and Astrophysics, 458 (2): 609–623, arXiv:astro-ph/0608160, Bibcode:2006A&A...458..609D, doi:10.1051/0004-6361:20065105, S2CID 9341088.

[aaa421_241-5] Setiawan, J.; et al. (July 2004), "Precise radial velocity measurements of G and K giants. Multiple systems and variability trend along the Red Giant Branch", Astronomy and Astrophysics, 421: 241–254, Bibcode:2004A&A...421..241S, doi:10.1051/0004-6361:20041042-1.

[SIMBAD-6] "20 Boo". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved May 8, 2019.

[Eggleton2008-7] 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.

[Lepine2005-8] 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.

[Alves2000-9] Alves, David R. (August 2000), "K-Band Calibration of the Red Clump Luminosity", The Astrophysical Journal, 539 (2): 732–741, arXiv:astro-ph/0003329, Bibcode:2000ApJ...539..732A, doi:10.1086/309278, S2CID 16673121

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20 Boötis

References

External links

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