Eta Pegasi
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Eta Pegasi or η Pegasi, formally named Matar Template:IPAc-en,[11][12] is a binary star in the constellation of Pegasus. The apparent visual magnitude of this star is +2.95,[2] making it the fifth-brightest member of Pegasus. Based upon parallax measurements, the distance to this star is about Script error: No such module "convert". from the Sun.[1]
Nomenclature
η Pegasi (Latinised to Eta Pegasi) is the star's Bayer designation.
It bore the traditional name Matar, derived from the Arabic سعد المطر Saʽd al Maṭar, meaning lucky star of rain.[13] In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN)[14] to catalogue and standardize proper names for stars. The WGSN approved the name Matar for this star on 21 August 2016 and it is now so entered in the IAU Catalog of Star Names.[12]
In Chinese, Script error: No such module "Lang". (Script error: No such module "Lang".), meaning Resting Palace, refers to an asterism consisting η Pegasi, λ Pegasi, μ Pegasi, ο Pegasi, τ Pegasi and ν Pegasi.[15] Consequently, η Pegasi itself is known as Script error: No such module "Lang". (Script error: No such module "Lang".), "the Fourth Star of Resting Palace".[16]
Namesake
USS Matar (AK-119) wasScript error: No such module "Unsubst". a United States Navy Crater class cargo ship named after the star.Script error: No such module "Unsubst".
Properties
The Eta Pegasi system consists of a pair of stars in a binary orbit with a period of 813 days and an eccentricity of 0.183.[7] The primary component is a bright giant star with a stellar classification of G2 II[3] and about three and a half times the mass of the Sun.[8] The interferometry-measured angular diameter of this star, after correcting for limb darkening, is 3.471 ± 0.027 mas,[8] which, at its estimated distance, equates to a physical radius of more than 24 times the radius of the Sun.[8] It is radiating 331[8] times the luminosity of the Sun from its expanded outer envelope at an effective temperature of 4,970 K.[8] The rotation rate of the star slowed as it expanded, so it has a projected rotational velocity of 1.7 km s−1 with an estimated rotation period of 818 days.[6]
The secondary component is an F-type main sequence star with a classification of F0 V.[3] The secondary star is 3.56 magnitudes fainter that the primary star at 700 nm.[17] There are also 2 class G stars further away that may or may not be physically related to the main pair.Script error: No such module "Unsubst".
References
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- ↑ Template:Cite Gaia EDR3
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- ↑ Template:Cite simbad
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- ↑ a b Script error: No such module "citation/CS1".
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- ↑ Template:In lang 中國星座神話, written by 陳久金. Published by 台灣書房出版有限公司, 2005, Template:ISBN.
- ↑ Template:In lang 香港太空館 - 研究資源 - 亮星中英對照表 Template:Webarchive, Hong Kong Space Museum. Accessed on line November 23, 2010.
- ↑ Script error: No such module "Citation/CS1".
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