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衝撃刺激によるOHマザー放射は,銀河の中心にある超新星残骸G359.1-0.05の輪郭を描いている
F Yusef-Zadeh1, K I Uchida, D Roberts
1Department of Physics and Astronomy, Northwestern University, Evanston, IL 60208, USA.
Science (New York, N.Y.)
|December 15, 1995
まとめ
天文学者は,銀河の中心殻 (G359.1-0.5) の近くで1720メガヘルツの延長されたヒドロキシル (OH) マザー放射を検出しました. この発見は,超新星残骸の膨張による衝撃活動がOHマザー線を誘発するという理論を支持する.
科学分野:
- 天文学と天体物理学について
- ラジオ天文学 ラジオ天文学
- 星間媒介は,星間媒介である.
背景:
- 1720メガヘルツのヒドロキシル (OH) マザーラインは,星間媒質における衝撃活動の潜在的トレーサーである.
- 銀河の中央地域の非熱的無線連続源は,エネルギー現象の研究のターゲットです.
- 超新星残骸が分子雲と相互作用すると,衝撃波が生成されます.
研究 の 目的:
- 銀河の中心にある非熱的な無線連続源からの1720メガヘルツOHマザー線放射を調査するために.
- 超新星残骸に関連したマザー放出と衝撃活動との関係を調査する.
- OHマザーの衝突ポンプに必要な条件を特定する.
主な方法:
- Very Large Array (VLA) を利用して,無線観測を行った.
- 1720 メガヘルツ OH マザーラインの放射を検索しました.
- マザー特徴,連続体殻,分子ガスの間の空間的相関を分析した.
主要な成果:
- 連続体シェルG359.1-0.5のインターフェースに沿って1720メガヘルツOHマザー放射の拡大とコンパクトが検出され,周囲の高速分子ガスを取り囲んでいます.
- 中性ガス,非熱殻,およびマザー特徴の間の形態学的相関が観察されました.
- 周囲の分子雲とOHマザー斑点の間の有意な放射速度差 (>50 km/s) が発見されました.
結論:
- 観測されたOHマザー放射は,膨張する超新星残骸が分子物質に衝撃を与えるガスから発生するという仮説を強く支持しています.
- 1720メガヘルツのOHラインの衝突式ポンプの物理的条件は,残骸の末端にある一酸化炭素ガスの特定の低放射速度成分によって満たされている可能性が高い.
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