銀河の中心:異常な源の相互作用するシステム

Yusef-Zadeh¹, Melia, Wardle

¹Department of Physics and Astronomy, Northwestern University, Evanston, IL 60208, USA. E-mail: zadeh@nwu.edu. Department of Physics and Steward Observatory, The University of Arizona, Tucson, AZ 85721, USA. E-mail: melia@as.arizona.edu. S.

Science (New York, N.Y.)

|December 30, 1999

まとめ

ミルクウェイは銀河系です.

科学分野:

天体物理学と銀河研究センターの研究
恒星力学とブラックホール物理学

背景:

10光年以内の銀河の中心には,5つの重要な構成要素がある:超大質量ブラックホール候補 (射手座A*),進化した恒星と若い恒星,ガス雲,超新星残骸.
これらの構成要素は,深い重力潜力の井戸の中で相互作用し,銀河の中心部の現象を駆動します.

研究の目的:

銀河の中心における構成要素の相互作用の統合的なモデルを開発する.
銀河の核とブラックホールの特徴の理解を深めるために.

主な方法:

観測天文学と天体物理モデリングは,銀河中心の構成要素を研究するために使用されました.
分析は,射手座A*と周りの恒星とガス元素の相互作用に焦点を当てた.

主要な成果:

射手座A*の質量は,太陽質量2.6 +/- 0.2 x 10^6です. 射手座A*の質量は,太陽質量2.6 +/- 0.2 x 10^6です.
射手座A*によって観測された恒星風の増殖からの放射は,現在の銀河核モデルによって予測されたよりも低い.

結論:

銀河の中心内の複雑な相互作用は,銀河の核を理解するために不可欠です.
射手座A*増量放射線の不一致は,現在のブラックホールモデルにおけるギャップを強調しています.

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