Astronomy:Gamma Librae
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| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Libra |
| Right ascension | 15h 35m 31.57881s[1] |
| Declination | −14° 47′ 22.3278″[1] |
| Apparent magnitude (V) | +3.91[2] |
| Characteristics | |
| Spectral type | G8.5 III[3] |
| Astrometry | |
| Radial velocity (Rv) | −26.71[4] km/s |
| Proper motion (μ) | RA: +65.34[1] mas/yr Dec.: +7.45[1] mas/yr |
| Parallax (π) | 19.99 ± 0.20[1] mas |
| Distance | 163 ± 2 ly (50.0 ± 0.5 pc) |
| Absolute magnitude (MV) | −1.59[5] |
| Details[4] | |
| γ Lib A | |
| Mass | 1.15 M☉ |
| Radius | 11.14 R☉ |
| Luminosity | 72 L☉ |
| Surface gravity (log g) | 2.81±0.18[6] cgs |
| Temperature | 4826±48[6] K |
| Metallicity [Fe/H] | −0.26±0.03[6] dex |
| Rotational velocity (v sin i) | 1.60 km/s |
| Age | 4.31 Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
Gamma Librae (γ Librae, abbreviated Gamma Lib, γ Lib) is a suspected[8] binary star system in the constellation of Libra. It is visible to the naked eye, having an apparent visual magnitude of +3.91.[2] Based upon an annual parallax shift of 19.99 mas as seen from Earth, it lies 163 light years from the Sun.
The primary component (designated Gamma Librae A) has been formally named Zubenelhakrabi /zuːˌbɛnɛlˈhækrəbi/, the traditional name of the system.[9]
Nomenclature
γ Librae (Latinised to Gamma Librae) is the system's Bayer designation. The designations of the two components as Gamma Librae A and B derive from the convention used by the Washington Multiplicity Catalog (WMC) for multiple star systems, and adopted by the International Astronomical Union (IAU).[10]
Gamma Librae bore the traditional name Zuben (el) Hakrabi (also rendered as Zuben-el-Akrab and corrupted as Zuben Hakraki). The name is a modification of the Arabic زبانى العقرب Zubān al-ʿAqrab "the claws of the scorpion", a name that dates to before Libra was a distinct constellation from Scorpius.[citation needed] In 2016, the IAU organized a Working Group on Star Names (WGSN)[11] to catalog and standardize proper names for stars. The WGSN decided to attribute proper names to individual stars rather than entire multiple systems.[12] It approved the name Zubenelhakrabi for the component Gamma Librae A on 5 September 2017 and it is now so included in the List of IAU-approved Star Names.[9]
In Chinese, 氐宿 (Dī Xiù), meaning Root, refers to an asterism consisting of Gamma Librae, Alpha2 Librae, Iota Librae and Beta Librae.[13] Consequently, the Chinese name for Gamma Librae itself is 氐宿三 (Dī Xiù sān), "the Third Star of Root".[14]
Properties
Because the star lies near the ecliptic it is subject to occultations by the Moon, allowing the angular size to be measured.[15] As of 1940, the pair had an angular separation of 0.10 arc seconds along a position angle of 191°.[16]
The yellow-hued primary, component Aa, is an evolved G-type giant star with a stellar classification of G8.5 III[3] and an estimated age of 4.3 billion years. It has 1.15 times the mass of the Sun and has expanded to 11.14 times the Sun's radius. The star is radiating around 72 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,786 K.[4] There is a magnitude 11.2 visual companion, component B, at an angular separation of 42.5 arc seconds along a position angle of 157°, as of 2013.[16]
At its distance, the visual magnitude is diminished by an extinction of 0.11 due to interstellar dust.[2] The system is moving closer to the Sun with a radial velocity of −26.71 km/s.[4]
Planetary system
On the 11th of April 2018 the discovery of two gas giant planets orbiting Gamma Librae was announced. [17]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | — | 1.24 | 415.2 | 0.21 ± 0.10 | — | — |
| c | — | 2.17 | 964.6 ± 3.1 | 0.057 | — | — |
References
- ↑ 1.0 1.1 1.2 1.3 1.4 van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics 474 (2): 653–664, doi:10.1051/0004-6361:20078357, Bibcode: 2007A&A...474..653V.
- ↑ 2.0 2.1 2.2 Takeda, Yoichi et al. (August 2008), "Stellar Parameters and Elemental Abundances of Late-G Giants", Publications of the Astronomical Society of Japan 60 (4): 781–802, doi:10.1093/pasj/60.4.781, Bibcode: 2008PASJ...60..781T.
- ↑ 3.0 3.1 Keenan, Philip C.; McNeil, Raymond C. (1989), "The Perkins catalog of revised MK types for the cooler stars", Astrophysical Journal Supplement Series 71: 245, doi:10.1086/191373, Bibcode: 1989ApJS...71..245K.
- ↑ 4.0 4.1 4.2 4.3 Jofré, E. et al. (February 2015), "Stellar parameters and chemical abundances of 223 evolved stars with and without planets", Astronomy & Astrophysics 574: 46, doi:10.1051/0004-6361/201424474, A50, Bibcode: 2015A&A...574A..50J.
- ↑ Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters 38 (5): 331, doi:10.1134/S1063773712050015, Bibcode: 2012AstL...38..331A.
- ↑ 6.0 6.1 6.2 Marfil, E.; Tabernero, H. M.; Montes, D.; Caballero, J. A.; Soto, M. G.; González Hernández, J. I.; Kaminski, A.; Nagel, E. et al. (2020), "Stellar atmospheric parameters of FGK-type stars from high-resolution optical and near-infrared CARMENES spectra", Monthly Notices of the Royal Astronomical Society 492 (4): 5470–5507, doi:10.1093/mnras/staa058
- ↑ "HD 138905 -- Double or multiple star". SIMBAD Astronomical Database. http://simbad.u-strasbg.fr/sim-id.pl?protocol=html&Ident=gamma+librae. Retrieved 2007-01-22.
- ↑ Eggleton, P. P.; Tokovinin, A. A. (2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society 389 (2): 869, doi:10.1111/j.1365-2966.2008.13596.x, Bibcode: 2008MNRAS.389..869E.
- ↑ 9.0 9.1 "Naming Stars". IAU.org. https://www.iau.org/public/themes/naming_stars/. Retrieved 16 December 2017.
- ↑ Hessman, F. V.; Dhillon, V. S.; Winget, D. E.; Schreiber, M. R.; Horne, K.; Marsh, T. R.; Guenther, E.; Schwope, A.; Heber, U. (2010). "On the naming convention used for multiple star systems and extrasolar planets". arXiv:1012.0707 [astro-ph.SR].
- ↑ "IAU Working Group on Star Names (WGSN)". https://www.iau.org/science/scientific_bodies/working_groups/280/. Retrieved 22 May 2016.
- ↑ "WG Triennial Report (2015-2018) - Star Names". p. 5. https://www.iau.org/static/science/scientific_bodies/working_groups/280/wg-starnames-triennial-report-2015-2018.pdf. Retrieved 2018-07-14.
- ↑ (in Chinese) 中國星座神話, written by 陳久金. Published by 台灣書房出版有限公司, 2005, ISBN:978-986-7332-25-7.
- ↑ (in Chinese) 香港太空館 - 研究資源 - 亮星中英對照表 , Hong Kong Space Museum. Accessed on line November 23, 2010.
- ↑ White, Nathaniel M.; Feierman, Barry H. (September 1987), "A Catalog of Stellar Angular Diameters Measured by Lunar Occultation", Astronomical Journal 94: 751, doi:10.1086/114513, Bibcode: 1987AJ.....94..751W.
- ↑ 16.0 16.1 Mason, B. D. et al. (2014), "The Washington Visual Double Star Catalog", The Astronomical Journal 122 (6): 3466–3471, doi:10.1086/323920, Bibcode: 2001AJ....122.3466M
- ↑ "Planets around the evolved stars 24 Booties and γ Libra: A 30d-period planet and a double giant-planet system in possible 7:3 MMR". Takuya Takarada, Bun'ei Sato, Masashi Omiya, Hiroki Harakawa, Makiko Nagasawa, Hideyuki Izumiura, Eiji Kambe, Yoichi Takeda, Michitoshi Yoshida, Yoichi Itoh, Hiroyasu Ando, Eiichiro Kokubo, Shigeru Ida (April 11, 2018).
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