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|- ! style="background-color: #FFFFC0;" colspan="2" | Characteristics |- | Spectral type | F (primary)/M (b)〔 |- style="vertical-align: top;" | Apparent magnitude (infrared, I band) | 15.40 (system)〔 |- style="vertical-align: top;" | Variable type | Eclipsing binary |- ! style="background-color: #FFFFC0;" colspan="2" | Astrometry |- style="vertical-align: | Distance | 5000 ± 1000 ly (1600 ± 400 pc)〔 |- ! style="background-color: #FFFFC0;" colspan="2" | Binary orbit |- style="vertical-align: top;" | Period (P) | 1.804〔Radius and mass of a transiting M dwarf near the hydrogen-burning limit. OGLE-TR-123, F. Pont, C. Moutou, F. Bouchy, R. Behrend, M. Mayor, S. Udry, D. Queloz, N. Santos, and C. Melo, ''Astronomy and Astrophysics'' 447, #3 (March 1, 2006), pp. 1035–1039. . .〕 days |- style="vertical-align: top;" | Eccentricity (e) | 0〔 |- style="vertical-align: top;" | Semi-major axis | 0.031 ± 0.002 AU〔 |- style="vertical-align: top;" | Inclination (i) | 86–90° 〔 OGLE-TR-123 is a binary stellar system containing one of the smallest main-sequence stars whose radius has been measured. It was discovered when the Optical Gravitational Lensing Experiment (OGLE) survey observed the smaller star eclipsing the larger primary. The orbital period is approximately 1.80 days.〔 The smaller star, OGLE-TR-123b, is estimated to have a radius around 0.13 solar radii, and a mass of around 0.085 solar masses (), or approximately 90 times Jupiter's. OGLE-TR-123b's mass is close to the lowest possible mass, estimated to be around 0.07 or 0.08 , for a hydrogen-fusing star.〔(Theory of Low-Mass Stars and Substellar Objects ), Gilles Chabrier and Isabelle Baraffe, ''Annual Review of Astronomy and Astrophysics'' 38 (2000), pp. 337–377.〕 OGLE-TR-123b is the second star with mass less than 0.1 whose radius has been directly measured; the first such star was the similar OGLE-TR-122b.〔 ==References== bg:OGLE-TR-122b pl:OGLE-TR-122b sk:OGLE-TR-122b 抄文引用元・出典: フリー百科事典『 ウィキペディア（Wikipedia）』 ■ウィキペディアで「OGLE-TR-123」の詳細全文を読む スポンサード リンク
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