翻訳と辞書 Words near each other ・ V352 Aurigae ・ V354 Cephei ・ V357 Carinae ・ V36 ・ V372 Carinae ・ V373 Cassiopeiae ・ V373 Scuti ・ V376 Carinae ・ V378 Normae ・ V380 Orionis ・ V381 Cephei ・ V382 Carinae ・ V382 Velorum ・ V385 Andromedae ・ V3903 Sagittarii ・ V391 Pegasi ・ V391 Pegasi b ・ V394 Aurigae ・ V399 Carinae ・ V3g ・ V4 ・ V4 engine ・ V40 ・ V40 Mini-Grenade ・ V404 Cygni ・ V4046 Sagittarii ・ V4199 Sagittarii ・ V420 Aurigae ・ V424 Lacertae ・ V433 Aurigae Dictionary Lists mini英和辞書 mini和英辞書 Webster 1913 Latin-English FOLDOC Wikipedia English ウィキペディア

翻訳と辞書　辞書検索 [ 開発暫定版 ] スポンサード リンク V391 Pegasi ： ウィキペディア英語版 V391 Pegasi V391 Pegasi, also catalogued as HS 2201+2610, is a blue-white subdwarf star approximately 4,570 light-years away in the constellation of Pegasus. The star is classified as an "extreme horizontal branch star". It is small, with only half the mass and a bit less than one-quarter the diameter of the Sun. It has luminosity 15.4 times the Sun. It could be quite old, perhaps in excess of 10 Gyr. It is a pulsating variable star of the V361 Hydrae type (or also called sdBVr type). ==Formation== Subdwarf B stars such as V391 Pegasi are thought to be the result of the ejection of the hydrogen envelope of a red giant star at or just before the onset of helium fusion. The ejection left only a tiny amount of hydrogen on the surface - less than 1/1000 of the total stellar mass. The future for the star is to eventually cool down to make a low mass white dwarf. Most stars retain more of their hydrogen after the first red giant phase, and eventually become asymptotic giant branch stars. The reason that some stars, like V391 Pegasi, lose so much mass is not well known. 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「V391 Pegasi」の詳細全文を読む スポンサード リンク 翻訳と辞書 : 翻訳のためのインターネットリソース Copyright(C) kotoba.ne.jp 1997-2016. All Rights Reserved.