X線フラッシュXRF 060218からの相対論的なエジェクタと宇宙爆発の速度
A M Soderberg1, S R Kulkarni, E Nakar
1Caltech Optical Observatories 105-24, California Institute of Technology, Pasadena, California 91125, USA. ams@astro.caltech.edu
Nature
|September 1, 2006
まとめ
X線閃光 (XRF) とガンマ線爆発 (GRB) は,巨大な恒星からの珍しい超新星です. XRF 060218の観測は,相対論的な噴射生成が,典型的な超新星からそれらを区別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
- 宇宙の爆発,宇宙の爆発.
- 恒星の進化について
背景:
- 長期にわたるガンマ線爆発 (GRB) とX線閃光 (XRF) は,巨大な恒星の死に関連した珍しい,非常に明るい出来事です.
- GRB/XRFと超新星が起源を共有している一方で,それらの極端な明るさを区別する物理的メカニズムは不明のままです.
研究 の 目的:
- XRF 060218 (SN 2006aj) を分析することによって,X線フラッシュ (XRF) の性質を調査する.
- GRB/XRFと普通の超新星との主要な物理的な違いを理解するために.
主な方法:
- XRF 060218.8の無線とX線観測を行った.
- イベントのエネルギー出力とエジェクタ特性を分析した.
主要な成果:
- XRF 060218は,典型的な宇宙GRBよりもエネルギーが少なく,より一般的です.
- このイベントは,軽度の相対論的なエジェクタと,持続的なX線を放射する中央エンジンを示しています.
- 放出されたエネルギーは,およそ10^48 erg です.
結論:
- 相対論的な放出物の生成は,GRB/XRFと普通の超新星との主要な区別である.
- 中央エンジンの性質 (ブラックホールまたはマグネタール) は,XRF 060218.8.のようなより少ない明るさ,球形のイベントから典型的なGRBを区別することができます.
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