グリーゼ105とは - わかりやすく解説 Weblio辞書

グリーゼ105

出典: フリー百科事典『ウィキペディア（Wikipedia）』 (2023/04/05 16:00 UTC 版)

グリーゼ105（Gliese 105）或いはHR 753は、くじら座にある連星系である。太陽に近く、およそ24光年しか離れていない^[2]。しかし、近いにもかかわらず、最も明るい主星だけがかろうじて肉眼でみえるだけである。この星系には、惑星は発見されていない。

脚注

注釈

^ ^a ^b パーセクは1 ÷ 年周視差（秒）より計算、光年は1÷年周視差（秒）×3.2615638より計算

出典

^ “APOD: GL 105C: The Coolest Star?”. NASA (1995年9月20日). 2018年3月10日閲覧。
^ ^a ^b ^c ^d ^e ^f ^g “HD 16160 -- High proper-motion Star”. SIMBAD. CDS. 2018年7月12日閲覧。
^ ^a ^b ^c ^d Golimowski, D. A.; et al. (1995-10), “Hubble Space Telescope Observations of the Very Low Mass Companion to Gliese 105A”, Astrophysical Journal Letters 452: L125-L128, Bibcode: 1995ApJ...452L.125G, doi:10.1086/309723
^ ^a ^b ^c ^d ^e ^f ^g ^h ⁱ Golimowski, David A.; et al. (2000-10), “The Very Low Mass Component of the Gliese 105 System”, Astronomical Journal 120 (4): 2082-2088, arXiv:astro-ph/0006230, Bibcode: 2000AJ....120.2082G, doi:10.1086/301567
^ Mason, Brian D.; et al. (2018-02), “The Washington Visual Double Star Catalog”, VizieR On-line Data Catalog: B/wds, Bibcode: 2018yCat....102026M
^ ^a ^b ^c ^d ^e ^f Reid, I. Neill; Gizis, John E. (1997-06), “Low-Mass Binaries and the Stellar Luminosity Function”, Astronomical Journal 113: 2246-2269, Bibcode: 1997AJ....113.2246R, doi:10.1086/118436
^ Heintz, Wulff D.; Cantor, Bruce A. (1994-04), “An astrometric study of four binary stars”, Publications of the Astronomical Society of the Pacific 106 (698): 363-364, Bibcode: 1994PASP..106..363H, doi:10.1086/133386
^ Golimowski, D. A.; et al. (1995-05), “Detection of a very low mass companion to the astrometric binary Gliese 105A”, Astrophysical Journal 444 (2): L101-L104, Bibcode: 1995ApJ...444L.101G, doi:10.1086/187870
^ ^a ^b ^c ^d Bessel, M. S. (1990-05), “BVRI photometry of the Gliese Catalogue stars”, Astronomy & Astrophysics Supplement Series 83 (2): 357-378, Bibcode: 1990A&AS...83..357B
^ ^a ^b ^c ^d Leggett, S. K. (1992-09), “Infrared colors of low-mass stars”, Astrophysical Journal Supplement Series 82 (1): 351-394, Bibcode: 1992ApJS...82..351L, doi:10.1086/191720
^ ^a ^b Samus, N. N.; et al. (2009-01), “General Catalogue of Variable Stars”, VizieR On-line Data Catalog: B/gcvs, Bibcode: 2009yCat....102025S
^ ^a ^b Gray, R. O.; et al. (2003-10), “Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 Parsecs: The Northern Sample. I”, Astronomical Journal 126 (4): 2048-2059, Bibcode: 2003AJ....126.2048G, doi:10.1086/378365
^ ^a ^b Reid, I. Neill; Hawley, Suzanne L.; Gizis, John E. (1995-10), “The Palomar/MSU Nearby-Star Spectroscopic Survey. I. The Northern M Dwarfs -Bandstrengths and Kinematics”, Astronomical Journal 110: 1838-1859, Bibcode: 1995AJ....110.1838R, doi:10.1086/117655
^ ^a ^b ^c Newton, Elizabeth R.; et al. (2015-02), “An Empirical Calibration to Estimate Cool Dwarf Fundamental Parameters from H-band Spectra”, Astrophysical Journal 800 (2): 85, Bibcode: 2015ApJ...800...85N, doi:10.1088/0004-637X/800/2/85
^ ^a ^b Mann, Andrew W.; et al. (2015-05), “How to Constrain Your M Dwarf: Measuring Effective Temperature, Bolometric Luminosity, Mass, and Radius”, Astrophysical Journal 804 (1): 64, arXiv:1501.01635, Bibcode: 2015ApJ...804...64M, doi:10.1088/0004-637X/804/1/64
^ ^a ^b ^c ^d ^e ^f ^g Önehag, A.; et al. (2012-06), “M-dwarf metallicities. A high-resolution spectroscopic study in the near infrared”, Astronomy & Astrophysics 542: A33, Bibcode: 2012A&A...542A..33O, doi:10.1051/0004-6361/201118101
^ Tokovinin, A. (2008-09), “Comparative statistics and origin of triple and quadruple stars”, Monthly Notices of the Royal Astronomical Society 389 (2): 925-938, Bibcode: 2008MNRAS.389..925T, doi:10.1111/j.1365-2966.2008.13613.x
^ “Hubble Spies a Really Cool Star”. HubbleSite (1995年9月14日). 2018年3月10日閲覧。