銀河NGC 7793の強力なマイクロクワザーの周りに300パーセル長さのジェットで膨らんだバブル
Manfred W Pakull1, Roberto Soria, Christian Motch
1University of Strasbourg, CNRS UMR 7550, Observatoire Astronomique, 11 rue de l'Université, F67000 Strasbourg, France. manfred.pakull@astro.unistra.fr
Nature
|July 9, 2010
まとめ
私たちはNGC 7793でマイクロクワザールS26を発見し,SS433に似ているがより大きな強力なジェットを持っています. そのジェットは,そのX線核放射よりも1万倍エネルギーが強い.
科学分野:
- * 天体物理学
- * 高エネルギー天体物理学
- * ブラックホール物理学
背景:
- * ブラックホールの蓄積状態は,エディントン光度に近いかそれ以上のもので,源が稀であるため,ほとんど理解されていません.
- *超光るX線源 (ULXs) は,超核のブラックホールで,超エディントン速さで膨張している可能性が高い.
- * 恒定ジェットを持つマイクロクワザーはULXよりも明るくなく,ULXには通常,コリマートジェットの証拠がない.
研究 の 目的:
- *NGC 7793.3にある大きな星雲S26の性質を調査する.
- * S26がコリマートジェットを持つブラックホールから電力を供給されているかどうかを判断する.
- * S26の出力力と構造を特徴付け,既知の天体物理学的情報源と比較する.
主な方法:
- *S26星雲とその核からのX線と光学データの分析.
- *ジェットの機械的出力量の決定.
- * S26の構造分析で,ファナロフ・ライリー型II活性銀河とマイクロクワザールと比較した.
主要な成果:
- * S26はブラックホールから2つのコリマートジェットが生成される.
- *ジェットの機械的力は,X線核放射の約10^40 erg s^-1~10^4倍である.
- * S26は,X線ホットスポット,ラジオロブ,X線コクーンを含むファナロフ・ライリー型II構造を示しています.
結論:
- *S26は強力なマイクロクワザールで,SS433よりも大きく,エネルギーが豊富です.
- * S26のジェット力のほとんどは,相対性電子ではなく,葉内の熱粒子として散らばります.
- *この発見は,超エディントン速度のブラックホールの蓄積状態に関する新しい洞察を提供します.
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