超大質量ブラックホールの周りの星形成

I A Bonnell¹, W K M Rice

¹Scottish Universities Physics Alliance, School of Physics and Astronomy, University of St. Andrews, North Haugh, St. Andrews, Fife KY16 9SS, UK. iab1@st-andrews.ac.uk

Science (New York, N.Y.)

|August 23, 2008

まとめ

超大質量ブラックホールの近くの巨大な分子雲は,奇妙なリングで星を形成することができます. 数学的シミュレーションでは,潮力と加熱による雲の断片化が示され,銀河の中心にある若い巨大な恒星が説明される.

科学分野:

* 天体物理学
* 計算による天体物理学
* 星の形成について

背景:

* 銀河の中心にある超大質量ブラックホール付近の偏心指輪に,若い質量のある恒星が観測されています.
* 既存の恒星形成理論は,高潮切断と輸送の課題により,それらの存在を説明するために苦労しています.

研究の目的:

* 超大質量ブラックホールの周りの奇妙なリングの若い巨大な星の形成メカニズムを調査する.
* 観測証拠と,極端な銀河環境における恒星形成の理論モデルを調和させる.

主な方法:

*超大質量ブラックホールと相互作用する巨大な分子雲の数値シミュレーション.
* エネルギー伝達,円盤の断片化,恒星の質量分布の分析.

主要な成果:

* 突入する分子雲は,超大質量ブラックホールの周りに束縛され,偏心的な円盤を形成することがあります.
*円盤の断片化と圧縮加熱により,比較的高質量星が形成される.
* シミュレーションした星は円盤の偏心性を継承し,観測された恒星輪を説明する可能性がある.

結論:

*巨大な分子雲の崩壊と断片化は,奇妙なリングで若い巨大な恒星を形成するための実行可能なメカニズムを提供します.
*この過程は,超大質量ブラックホールの近くに観測された複数の特異的な恒星輪の存在を説明できる.
*このモデルは,中央のブラックホールと雲の相互作用によって誘発される恒星形成の繰り返しサイクルを示唆しています.

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