巨大 な 伸び た 流線 が 大 量 の 若い 星 を 養い て いる
Fernando A Olguin1,2,3, Patricio Sanhueza4, Adam Ginsburg5
1Center for Gravitational Physics, Yukawa Institute for Theoretical Physics, Kyoto University, Kitashirakawa Oiwakecho, Sakyo-ku, Kyoto 606-8502, Japan.
Science advances
|August 20, 2025
まとめ
高質量なプロトスターは 円盤ではなく ストリーマーで形成されます これらのガスの流れは 恒星に直接物質を送り込み 恒星形成中のフィードバック効果を 制御する可能性があります
科学分野:
- 天文学
- 天体物理学
- 星の形成
背景:
- 恒星形成の環境は,原星質量蓄積に影響する.
- 原惑星円盤は,従来,原星へのガス蓄積の主要な場所と考えられています.
- 円盤は若い恒星の周りに どこにでも存在します
研究 の 目的:
- 原惑星円盤を超えた 代替的増殖メカニズムを調査する
- 高質量恒星形成中のガス流入の形態と役割を特徴付ける.
- 観測された流入がフィードバックに影響を与えるのに十分な増殖率を維持できるかどうかを判断する.
主な方法:
- アタカマの大型ミリメートル/サブミリメートル配列 (ALMA) の高解像度観測を用いて
- 観測データを分析してガスの流入構造を特定し,追跡する.
- 観測された流体の質量と流量を定量化します.
主要な成果:
- 円盤だけではなく 流れの形での流れの発見です
- ストリーマーが予想される円盤半径内に存在することが観察されました.
- これらのストリーマーは円盤の代わりとして働き 物質をプロトスターまたはコンパクトディスクに直接送ります
結論:
- ガス流は高質量プロトスターに 重要な役割を果たします
- ストリーマーは,蓄積過程で従来のディスクをバイパスまたは置き換えることができます.
- ストリーマー経由で観測された蓄積率は,若い質量のある恒星からのフィードバックを制御または消すのに十分である.
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