Eta Ophiuchi: Difference between revisions
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'''Eta Ophiuchi''' | '''Eta Ophiuchi''' is a [[binary star]] in the [[constellation]] of [[Ophiuchus]]. Its name is a [[Bayer designation]] that is [[Romanization of Greek|Latinized]] from '''η Ophiuchi''', and abbreviated Eta Oph or η Oph. With a combined [[apparent magnitude]] of +2.43, it is the second-brightest of the constellation and one of the [[list of brightest stars|brightest stars]] in the night sky. Based on [[stellar parallax|parallax]] measurements taken during the [[Hipparcos]] mission, it is approximately 88 [[light-year]]s away. | ||
The components of this system are designated {{nobr|Eta Ophiuchi A}} (also called '''Sabik''' {{IPAc-en|'|s|ei|b|I|k}}<ref name=Kunitzsch>{{cite book | |||
|last1=Kunitzsch |first1=Paul | |last1=Kunitzsch |first1=Paul | ||
|last2=Smart |first2=Tim | |last2=Smart |first2=Tim | ||
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|publisher = Sky Pub |location = Cambridge, Massachusetts | |publisher = Sky Pub |location = Cambridge, Massachusetts | ||
|isbn = 978-1-931559-44-7 | |isbn = 978-1-931559-44-7 | ||
}}</ref><ref name="IAU-LSN">{{cite web | url=https://www.iau.org/public/themes/naming_stars/ | title=Naming Stars |publisher=IAU.org |access-date=27 February 2018}}</ref> and | }}</ref><ref name="IAU-LSN">{{cite web | url=https://www.iau.org/public/themes/naming_stars/ | title=Naming Stars |publisher=IAU.org |access-date=27 February 2018}}</ref>), and {{nobr|Eta Ophiuchi B}}. | ||
==Nomenclature== | ==Nomenclature== | ||
Latest revision as of 21:24, 22 June 2025
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Eta Ophiuchi is a binary star in the constellation of Ophiuchus. Its name is a Bayer designation that is Latinized from η Ophiuchi, and abbreviated Eta Oph or η Oph. With a combined apparent magnitude of +2.43, it is the second-brightest of the constellation and one of the brightest stars in the night sky. Based on parallax measurements taken during the Hipparcos mission, it is approximately 88 light-years away.
The components of this system are designated Template:Nobr (also called Sabik Template:IPAc-en[9][10]), and Template:Nobr.
Nomenclature
η Ophiuchi (Latinised to Eta Ophiuchi) is the system's Bayer designation. WDS J17104-1544AB is its designation in the Washington Double Star Catalog. The designations of the two components as WDS J17104-1544 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).[11]
It bore the traditional name Sabik, from the Arabic السابق al-sābiq "the preceding one", of uncertain reference.[9] In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN)[12] to catalogue and standardize proper names for stars. The WGSN approved the name Sabik for the component WDS J17104-1544 A on 21 August 2016 and it is now so included in the List of IAU-approved Star Names.[10]
In Chinese, this star is considered part of Script error: No such module "Lang". (Script error: No such module "Lang".), meaning Left Wall of Heavenly Market Enclosure, which refers to an asterism representing eleven old states in China that mark the left borderline of the enclosure, consisting of Eta Ophiuchi, Delta Herculis, Lambda Herculis, Mu Herculis, Omicron Herculis, 112 Herculis, Zeta Aquilae, Theta Serpentis, Eta Serpentis, Nu Ophiuchi and Xi Serpentis.[13] Consequently, the Chinese name for Eta Ophiuchi itself is Script error: No such module "Lang". (Script error: No such module "Lang"., Template:Langx), representing the state Song (宋).[14][15]
Namesake
USS Sabik (AK-121) was a United States Navy Crater class cargo ship named after the star.
Properties
Eta Ophiuchi consists on two A-type main-sequence stars,[4] currently fusing hydrogen into helium at their core. The primary, of apparent magnitude +3.05,[3] has about 2.5 times the Sun's radius and 2.25 times its mass, with an effective temperature around 9,000 K.[4] The secondary, of apparent magnitude +3.27,[3] is 2 times as large and massive than the Sun, with an effective temperature of 8,700 K. The estimated age of the system is 500 million years, albeit with significant uncertainty.[4]
The stars take 87.8 years to complete an orbit, which is highly elliptical: While the semi-major axis is 31 astronomical units, the high orbital eccentricity of 0.931 take them to a distance of 2.15 au during their closest approach (the periastron); the last of such occurring in 2024. Such large eccentricity hindered accurate measurements of the stellar mass with the Kepler's third law, until observations with the Very Large Telescope during the most recent periastron accurately determined orbital elements such as the eccentricity, hence a considerable mass sum for A2V-type stars.[4]
References
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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.
- ↑ Template:In lang English-Chinese Glossary of Chinese Star Regions, Asterisms and Star Name Template:Webarchive, Hong Kong Space Museum. Accessed on line November 23, 2010.