コマ銀河団の中心にある線形構造
J S Sanders1, A C Fabian, E Churazov
1Max-Planck-Institut für Extraterrestrische Physik, Giessenbachstrasse 1, 85748 Garching, Germany. jsanders@mpe.mpg.de
まとめ
銀河団のコアは大規模な構造を示し,渦巻理論に挑戦しています. ディープ・チャンドラによるX線観測は,長寿で低エントロピーな腕を明らかにし,磁場による抑制された乱流と伝導を示唆している.
科学分野:
- 天体物理学 天体物理学
- 銀河団の銀河団は銀河団を構成している.
- プラズマ物理学 プラズマ物理学
背景:
- 銀河団には,熱いX線を放射するプラズマが含まれています.
- このプラズマの乱流運動は,エネルギー密度に大きく貢献すると予測されています.
- プラズマダイナミクスを理解することは,クラスターの進化にとって極めて重要です.
研究 の 目的:
- コマ星群の核中のプラズマの構造と動態を調査する.
- 観察されたプラズマ構造の寿命と起源を決定する.
- これらの構造が渦巻と伝導に与える影響を評価する.
主な方法:
- ディープ・チャンドラX線観測所によるコマ星団の観測.
- 150キロパーセックスをカバーする準線形高密度の腕の分析.
- 合併したサブクラスターから取り除かれた可能性が高い低エントロピーの材料を追跡する.
主要な成果:
- コマ星群の中核に広大で一貫した低エントロピー腕を発見.
- これらの腕と合併する銀河のサブグループとの間の接続の識別.
- 何億年にもわたる一貫性の証拠.
結論:
- 観測された構造は,クラスター・コアにおける抑制された同位流動の乱れと伝導を暗示しています.
- 磁場は,乱流と伝導を抑制する責任を負う可能性が高い.
- これらの発見は,過去10億年のサブクラスター合併活動に関する洞察を提供します.
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