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大マゲラン雲の巨大な若い星からのパーセックスケールの光学ジェット
Anna F McLeod1, Megan Reiter2, Rolf Kuiper3
1School of Physical and Chemical Sciences, University of Canterbury, Christchurch, New Zealand.
Nature
|January 25, 2018
まとめ
天文学者は HH 1177 を発見しました 大型マゲラン雲の 巨大な若い星からの光学ジェットです この発見は ジェット発射とコリマーションの物理が 恒星の質量に関係なく 普遍的であることを示唆しています
科学分野:
- 天体物理学
- スター進化
- 星の形成
背景:
- 若い恒星物体 (YSO) は,通常,蓄積円盤と関連付けられている高度にコリマートされたジェットを示します.
- 高質量恒星では円盤媒介の蓄積がますます明らかになっているが,その形成は不明である.
- 以前は,巨大な恒星からのジェットは,光学波長や銀河系外では観測されませんでした.
研究 の 目的:
- 銀河系の外にある 巨大な恒星から 光学的にイオン化されたジェットが 発見されたことを報告する
- 巨大な恒星形成の理論に このジェットの性質と意味を調査する
- ジェット発射とコリマーションの物理は 恒星の質量とは無関係だという仮説を テストするために
主な方法:
- HH1177ジェットの光学観測
- ジェットのコリマーション,幾何学,起源の分析.
- 低質量の若い恒星物体からの既知のジェットと比較.
主要な成果:
- HH1177の発見, 高度合体,双極光学イオン化ジェット.
- このジェットは 大型マゲラン雲の 巨大な若い恒星物体から発生します
- ジェットは少なくとも10パーセックに及ぶ 継続的な円盤媒介の蓄積を示しています
結論:
- 観測されたジェットは,巨大な恒星における円盤媒介の蓄積の証拠を提供します.
- このシステムの形成は,低質量恒星形成のメカニズムを拡大したものです.
- ジェット発射とコリマーションを制御する物理学は 恒星質量とは独立しているようです
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