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Kepler-70 (formerly called KOI-55) is a star in the constellation Cygnus with an apparent visual magnitude of 14.87.〔 This is too faint to be seen with the naked eye; viewing it requires a telescope with an aperture of or more.〔 A subdwarf B star, KOI-55 passed through the red giant stage some 18.4 million years ago. In its present day state, it is fusing helium in its core. Once it runs out of helium it will contract to form a white dwarf. It has a relatively small radius of about 0.2 times the Sun's radius; white dwarfs are generally much smaller. The star is host to a planetary system with two planets, KOI-55.01 and KOI-55.02.〔 == Planetary system == On December 26, 2011, evidence for two extremely short-period planets was announced. They were detected by the reflection of starlight caused by the planets themselves, rather than through a variation in apparent stellar magnitude caused by them transiting the star. The measurements also suggested a smaller body between the two confirmed planets; this remains unconfirmed. Orbits of Kepler-70b and Kepler-70c have 7:10 orbital resonance and have the closest approach between planets of any known planetary system. 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「Kepler-70」の詳細全文を読む スポンサード リンク
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