コンパクトバイナリ合併によるギガ電子ボルトの排出量

Alessio Mei^1,2, Biswajit Banerjee^3,4, Gor Oganesyan^3,4

¹Gran Sasso Science Institute, L'Aquila, Italy. alessio.mei@gssi.it.

Nature

|December 8, 2022

まとめ

長期ガンマ線爆発 (GRB) は,コンパクトバイナリ融合と関連していました. 予期せぬ高エネルギーガンマ線放射が観測され,おそらくキロノヴァ光子による逆コンプトン散乱によるものであった.

科学分野:

天体物理学
高エネルギー天体物理学
重力波天文学

背景:

ガンマ線爆発 (GRB) は通常巨大な星の崩壊と関連しています
GRB 211211Aは長い期間にもかかわらず,光学赤外線キロノヴァの放射を示し,コンパクトな二重結合の起源を示唆しました.
標準的な照明モデルでは,GRBからの遅い時間の放射を完全に説明できません.

研究の目的:

GRB 211211Aからの高エネルギーガンマ線放射の起源を調査する.
観測された放射は標準的な後照明モデルで説明できるのか,それとも別の説明が必要なのかを判断する.
コンパクトバイナリ合併を理解するためのこれらの発見の含意を探求する.

主な方法:

GRB 211211Aの多波長観測,公開データと専用データを含む.
ガンマ線放射の詳細なモデリング,観測と理論的な後光予測を比較する.
逆コンプトン散乱のような潜在的な放出メカニズムの分析.

主要な成果:

GRB 211211Aから高エネルギーガンマ線放射 (0.1 GeV以上) が検出され,爆発から1000秒後に始まった.
遅い時期に観測されたガンマ線流は,標準的な後光モデルからの予測を超えました.
キロノバ放射は,逆コンプトン散乱のための潜在的な種子光子の源として特定されました.

結論:

GRB 211211Aからの高エネルギー放出は,標準的な後発光プロセスによるものではありません.
キロノヴァ光子との遅い時間のジェットの相互作用による逆コンプトン放射は合理的な説明を提供している.
この発見は二重中性子星の合併に関連する現象について新たな洞察をもたらします

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