ヴェラパルサー風雲のX線はシンクロトロン限界に近い極化している

Fei Xie^1,2, Alessandro Di Marco³, Fabio La Monaca³

¹Guangxi Key Laboratory for Relativistic Astrophysics, School of Physical Science and Technology, Guangxi University, Nanning, China. xief@gxu.edu.cn.

Nature

|December 21, 2022

まとめ

パルサー風の星雲は高極化を示し,電子は均一な磁場の中で最小の乱れで加速します. この発見は,パルサー風の星雲の物理学の新しい洞察を提供します.

科学分野:

天体物理学
高エネルギー天体物理学
プラズマ物理学

背景:

パルサー風の星雲 (PWNe) は,パルサーが周囲の媒質に衝突する相対論的な粒子流出によって形成される.
パルサーB0833-45によって動いているベラパルサー風雲は,ベラX構造と超新星残骸の中に位置しています.
以前の研究では,X線で弧とジェットと,Vela PWNeの外部の領域のラジオ観測で高い極化を示しました.

研究の目的:

粒子加速と磁場特性を調査するヴェラパルサー風雲の内部の領域
パルサー風の星雲の条件と周辺の超新星残骸の条件を比較するためです

主な方法:

内部のヴェラパルサー風雲のX線観測.
シンクロトロン放出と極化特性の分析.

主要な成果:

X線観測では,内側の星雲の先端の極化が60%を超え,シンクロトロン放射の理論的限界に近づいていることが明らかになった.
推論された条件は,PWNe内の非常に均一な磁場の中で電子が最小の乱れで加速することを示唆しています.

結論:

ヴェラパルサー風雲の電子加速機構は,超新星残骸のそれと大きく異なる.
この発見は,パルサー風の星雲内の高度に秩序付けられた磁場における効率的な粒子加速のモデルを支持する.

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