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Lambda Aquilae
Lambda Aquilae (λ Aql, λ Aquilae) is a star in the constellation Aquila. It has the traditional name Al Thalimain, which it shares with ι Aquilae. The name is derived from the Arabic الثالمين ''al-thalīmain'' "the two ostriches". Lambda Aquilae is more precisely ''Al Thalimain Prior''. It has an apparent visual magnitude of 3.43,〔 which is bright enough to be seen with the naked eye. Parallax measurements place it at a distance of about from Earth.〔
In Chinese, (), meaning ''Market Officer'', refers to an asterism consisting of λ Aquilae, α Scuti, δ Scuti, ε Scuti, β Scuti, η Scuti, 12 Aquilae, 15 Aquilae and 14 Aquilae.〔 ''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.〕 Consequently, λ Aquilae itself is known as (, (英語:the Seventh Star of Market Officer).)〔 (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.〕
==Properties==
Lambda Aquilae is a main sequence star with a stellar classification of B9Vn,〔 which means that, like the Sun, it is generating energy at its core through the nuclear fusion of hydrogen. It is more massive than the Sun, with about three times its mass, and radiates about 55〔 times the Sun's luminosity from its outer envelope at a higher effective temperature of 11,780 K.〔 This temperature gives Lambda Aquilae the blue-white hue that is a characteristic of B-type stars.〔 Lambda Aquilae was one of the least variable stars observed by the Hipparcos satellite. It is a suspected Lambda Boötis star〔 and has an age of about 160 million years.〔
This star lies about 5° from the galactic plane and about 30° from the line of sight to the Galactic Center. This region of the sky is crowded with other objects along the line of sight, with at least 55 located within 10 arcseconds of the star. Examination of the star shows no companions with an 85% probability.〔 Despite this, it is suspected of being a spectroscopic binary star.〔 That is, it may have an orbiting companion whose presence is revealed by displacements in the absorption lines in the spectrum caused by the Doppler effect. Based upon the width of these lines, the star is rotating rapidly, with a projected rotational velocity of .〔
抄文引用元・出典: フリー百科事典『 ウィキペディア（Wikipedia）』
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