|
The T Tauri wind — so named because of the young star currently in this stage—is a phenomenon indicative of the phase of stellar development between the accretion of material from the slowing rotating material of a solar nebula and the ignition of the hydrogen that has agglomerated into the protostar. The protostar at first only has about 1% of its final mass. But the envelope of the star continues to grow as infalling material is accreted. After 10,000–100,000 years, thermonuclear fusion begins in its core, then a strong stellar wind is produced which stops the infall of new mass. The protostar is now considered a young star since its mass is fixed, and its future evolution is now set. ==The evolutionary picture of low mass protostars== The T Tauri stars, with masses less than twice the mass of our Sun, are thought to follow this process: #very slowly rotating cloud solar nebula + trigger #collapse #star + protoplanetary disk formation #slow contraction and accretion + intense stellar winds (''bipolar flows'') #ignition of hydrogen burning and appearance of star on the ''main sequence''. 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「T Tauri wind」の詳細全文を読む スポンサード リンク
|