[{"@context":"http:\/\/schema.org\/","@type":"BlogPosting","@id":"https:\/\/wiki.edu.vn\/en\/wiki21\/hr-7135-wikipedia\/#BlogPosting","mainEntityOfPage":"https:\/\/wiki.edu.vn\/en\/wiki21\/hr-7135-wikipedia\/","headline":"HR 7135 – Wikipedia","name":"HR 7135 – Wikipedia","description":"before-content-x4 From Wikipedia, the free encyclopedia after-content-x4 Star in the constellation Aquila HR 7135 is a binary star system. Despite","datePublished":"2015-11-25","dateModified":"2015-11-25","author":{"@type":"Person","@id":"https:\/\/wiki.edu.vn\/en\/wiki21\/author\/lordneo\/#Person","name":"lordneo","url":"https:\/\/wiki.edu.vn\/en\/wiki21\/author\/lordneo\/","image":{"@type":"ImageObject","@id":"https:\/\/secure.gravatar.com\/avatar\/c9645c498c9701c88b89b8537773dd7c?s=96&d=mm&r=g","url":"https:\/\/secure.gravatar.com\/avatar\/c9645c498c9701c88b89b8537773dd7c?s=96&d=mm&r=g","height":96,"width":96}},"publisher":{"@type":"Organization","name":"Enzyklop\u00e4die","logo":{"@type":"ImageObject","@id":"https:\/\/wiki.edu.vn\/wiki4\/wp-content\/uploads\/2023\/08\/download.jpg","url":"https:\/\/wiki.edu.vn\/wiki4\/wp-content\/uploads\/2023\/08\/download.jpg","width":600,"height":60}},"image":{"@type":"ImageObject","@id":"https:\/\/en.wikipedia.org\/wiki\/Special:CentralAutoLogin\/start?type=1x1","url":"https:\/\/en.wikipedia.org\/wiki\/Special:CentralAutoLogin\/start?type=1x1","height":"1","width":"1"},"url":"https:\/\/wiki.edu.vn\/en\/wiki21\/hr-7135-wikipedia\/","wordCount":2856,"articleBody":"     (adsbygoogle = window.adsbygoogle || []).push({});before-content-x4From Wikipedia, the free encyclopedia       (adsbygoogle = window.adsbygoogle || []).push({});after-content-x4Star in the constellation AquilaHR 7135 is a binary star system. Despite its Flamsteed designation of 62 Serpentis, the star can be found in the equatorial constellation of Aquila,[10] in front of a dark rift in the Milky Way near the constellation border.[5] It is visible to the naked eye as a dim, yellow-hued point of light with an apparent visual magnitude of 5.57.[2] The system is located 283\u00a0light years distant from the Sun, based on parallax,[1] and is drifting further away with a radial velocity of 23\u00a0km\/s.[5]       (adsbygoogle = window.adsbygoogle || []).push({});after-content-x4Discovery of the binary nature of this system is credited to Canadian astronomer H. H. Plaskett in 1922. It is a single-lined spectroscopic binary with an orbital period of 8.2 years and an eccentricity of 0.24.[5][6] The visible component is an aging giant star with a stellar classification of G9\u00a0III,[3] having exhausted the supply of hydrogen at its core and expanded to 10.7[1] times the Sun’s radius. It is a red clump giant, indicating it is on the horizontal branch and is generating energy via core helium fusion.[11] The star is 3.2[7]\u00a0billion years old with 1.54[7] times the mass of the Sun. It is radiating 53[1] times the Sun’s luminosity from its enlarged photosphere at an effective temperature of 4,666\u00a0K.[7] The star has a very low rate of spin, with the projected rotational velocity being too small to measure.[8]References[edit]^ a b c d e f g h i j Brown, A. G. A.;  et\u00a0al. (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 Johnson, H. L.;  et\u00a0al. (1966), “UBVRIJKL photometry of the bright stars”, Communications of the Lunar and Planetary Laboratory, 4 (99): 99, Bibcode:1966CoLPL…4…99J.^ a b McWilliam, Andrew (December 1990), “High-resolution spectroscopic survey of 671 GK giants. I – Stellar atmosphere parameters and abundances”, Astrophysical Journal Supplement Series, 74: 1075\u20131128, Bibcode:1990ApJS…74.1075M, doi:10.1086\/191527^ a b 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\u00a0119257644.^ a b c d e Griffin, R. F. (1981), “Spectroscopic binary orbits from photoelectric radial velocities. Paper 41: HR 7135”, The Observatory, 101: 208\u2013211, Bibcode:1981Obs…101..208G.^ a b Jancart, S.;  et\u00a0al. (2005), “Astrometric orbits of SB9 stars”, Astronomy and Astrophysics, 442 (1): 365\u2013380, arXiv:astro-ph\/0507695, Bibcode:2005A&A…442..365J, doi:10.1051\/0004-6361:20053003, S2CID\u00a015123997.^ a b c d e f Luck, R. Earle (2015), “Abundances in the Local Region. I. G and K Giants”, Astronomical Journal, 150 (3), 88, arXiv:1507.01466, Bibcode:2015AJ….150…88L, doi:10.1088\/0004-6256\/150\/3\/88, S2CID\u00a0118505114.^ a b c d Massarotti, Alessandro;  et\u00a0al. (January 2008), “Rotational and Radial Velocities for a Sample of 761 HIPPARCOS Giants and the Role of Binarity”, The Astronomical Journal, 135 (1): 209\u2013231, Bibcode:2008AJ….135..209M, doi:10.1088\/0004-6256\/135\/1\/209.^ “HD 175515”. SIMBAD. Centre de donn\u00e9es astronomiques de Strasbourg. Retrieved 2019-08-04.^ Kaler, James B. (1996), The ever-changing sky: a guide to the celestial sphere, Cambridge University Press, p.\u00a0119, ISBN\u00a00-521-38053-7.^ Alves, David R. (August 2000), “K-Band Calibration of the Red Clump Luminosity”, The Astrophysical Journal, 539 (2): 732\u2013741, arXiv:astro-ph\/0003329, Bibcode:2000ApJ…539..732A, doi:10.1086\/309278, S2CID\u00a016673121.       (adsbygoogle = window.adsbygoogle || []).push({});after-content-x4"},{"@context":"http:\/\/schema.org\/","@type":"BreadcrumbList","itemListElement":[{"@type":"ListItem","position":1,"item":{"@id":"https:\/\/wiki.edu.vn\/en\/wiki21\/#breadcrumbitem","name":"Enzyklop\u00e4die"}},{"@type":"ListItem","position":2,"item":{"@id":"https:\/\/wiki.edu.vn\/en\/wiki21\/hr-7135-wikipedia\/#breadcrumbitem","name":"HR 7135 – Wikipedia"}}]}]