超光るX線源のブラックホールの質量は15太陽質量未満である

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C Motch¹, M W Pakull¹, R Soria²

¹Observatoire astronomique de Strasbourg, Université de Strasbourg, CNRS, UMR 7550, 11 rue de l'Université, F-67000 Strasbourg, France.

|October 10, 2014

まとめ

超光るX線源は,中等質量ブラックホールではないかもしれません. P13系にある恒星の質量のブラックホールは,超光る性質を示しており,超臨界の蓄積がこれらの現象を説明することを示唆しています.

科学分野:

天体物理学天体物理学
X線天文学 X線天文学
ブラックホール物理学ブラックホール物理学

背景:

超光るX線源 (ULXs) は,銀河の恒星質量ブラックホールとは異なる性質を示す.
その高輝度,柔らかいX線成分,スペクトルカットオフは,中等質量ブラックホールやスーパーエディントン増殖を含む議論の余地のある解釈につながった.
柔らかいX線スペクトルを持つ恒星質量ブラックホールの近年の観測は,再評価を促した.

研究の目的:

銀河NGC 7793.3にある超光るX線源P13の性質を調査する.
P13がULXsのカノニカルな性質を示すかどうかを判断する.
P13系におけるブラックホールの質量を制限し,それに伴う蓄積過程を理解する.

主な方法:

NGC 7793.3にあるX線源P13の観測と分析
ドナー星 (B9Ia) のX線加熱によって引き起こされる光学および紫外線変調をモデリングする.
ブラックホールの質量と蓄積特性を決定するためのスペクトル分析.

主要な成果:

X線源P13は,64日周期のバイナリ系にあることが判明しました.
P13は,超光X線源の3つの正規の特性をすべて示しています.
P13のブラックホールの質量は,太陽の質量15倍未満に制限されました.
P13における柔らかい熱放出とスペクトルの曲線は,超臨界の蓄積のサインである.

結論:

P13の発見は,巨大な恒星質量ブラックホールへの超臨界の蓄積がULXの性質を説明できることを示しています.
これは,以前は中等質量ブラックホールと考えられていたULXの代替説明を提供する.
巨大な恒星質量ブラックホールへの超臨界の蓄積は,数倍10^40エルグ/秒までの輝度を持つULXを説明できる.

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