超新星残骸の宇宙線加速効率の測定
E A Helder1, J Vink, C G Bassa
1Astronomical Institute Utrecht, Utrecht University, Post Office Box 80000, NL-3508 TA Utrecht, Netherlands. e.a.helder@uu.nl
まとめ
宇宙で最もエネルギッシュな粒子である宇宙線は,主に超新星残骸によって加速されます. この研究では,宇宙線が超新星残骸RCW86の衝撃後圧力の50%以上を占め,衝撃加熱機構に影響を与えていることが明らかになりました.
科学分野:
- 天体物理学 天体物理学
- 高エネルギー粒子物理学 高エネルギー粒子物理学
背景:
- 超新星残骸は,宇宙線加速の主要な候補である.
- 正確な加速メカニズムと効率は,まだ十分に理解されていない.
研究 の 目的:
- 超新星残骸の衝撃の背後にある圧力に対する宇宙線の貢献を調査する.
- 超新星残骸RCW 86.6の宇宙線含有量を決定する.
主な方法:
- 熱ドップラー拡大を測定するための光学スペクトロスコーピー.
- シンクロトロン放射と自己運動を分析するためのX線観測.
- 衝撃後の陽子温度と衝撃速度の比較.
主要な成果:
- コスミックレイの圧力は,RCW 86の北東の衝撃の背後にある熱圧を超えています.
- 超相対性電子がX線シンクロトロン放出を支配する.
- 宇宙線は,衝撃後の圧力の50%以上を占める.
結論:
- 標準的な衝撃加熱モデルは,RCW 86.の観測を説明するのに不十分です.
- 超新星残骸は,粒子を宇宙線エネルギーに大幅に加速することができます.
- これは,超新星残骸における宇宙線加速の直接的な証拠を提供します.
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