長い γ 線爆発からの逆コンプトン放射の観測
1Center for Space Plasma and Aeronomic Research, University of Alabama in Huntsville, Huntsville, AL, USA.
Nature
|November 22, 2019
まとめ
長時間続くガンマ線爆発 (GRB) は 独特で強力なテラ電子電圧の 放射成分を示しています 逆コンプトン散乱によって説明されます.
科学分野:
- 天体物理学
- 高エネルギー天体物理学
- ガンマ線天文学
背景:
- 長時間続くガンマ線爆発 (GRB) は 死にかけている巨大な星の相対論的ジェットから発生します
- 噴射中の即時放射 (keV-MeV) が発生し,噴射後の放射 (radio-GeV) は媒介との相互作用によって発生する.
- 後光は通常,外部の衝撃からのシンクロトロン放射によって説明されます.
研究 の 目的:
- 複数の周波数のGRB190114Cの観測を分析する
- 最近観測されたGRB 190114Cからの強烈なテラ電子電圧 (TeV) 放射の起源と性質を調査する.
- TeVの放出条件がGRBに共通しているかどうかを判断する.
主な方法:
- 複数の周波数のGRB 190114Cの観測
- 5 × 10−6から1012 eVまでのブロードバンドスペクトルエネルギー分布 (SED) の分析.
- シンクロトロン放射と逆コンプトン散乱を含む放射機構のモデリング.
主要な成果:
- GRB 190114CのブロードバンドSEDは,二重ピーク構造を示しています.
- シンクロトロンコンポーネントと比較できる独特のTeVスペクトルコンポーネントが特定されました.
- このTeVコンポーネントは後光と関連しており,シンクロトロン光子の逆コンプトン上方散乱によって説明される.
結論:
- 高エネルギー電子によるシンクロトロン光子の逆コンプトン散乱は,観測されたTeV放射に満足のいく説明を提供している.
- この放出に必要な条件はGRBの典型です.
- 逆コンプトン放射は,長時間のガンマ線爆発において一般的な現象である.
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