軟X線の検出と,ヘイル・ボップ彗星の高貴なガスの探査

V A Krasnopolsky¹, M J Mumma, M Abbott

¹Catholic University of America, Washington, DC 20064, USA. ys2VK@lepvax.gsfc.nasa.gov 20771, USA.

Science (New York, N.Y.)

|September 5, 1997

まとめ

ヘール・ボップ彗星

科学分野:

彗星科学は彗星科学である.
X線天文学X線天文学とは
アストロケミストリーアストロケミストリー

背景:

ヘイル・ボップ彗星 (C/1995 O1) は,柔らかいX線で観測される著名な彗星である.
以前の観測では,そのX線放射と元素組成の詳細な分析が欠けていた.

研究の目的:

ヘイル・ボップ彗星の柔らかいX線放射を分析するために.
彗星氷の元素組成を決定する.
彗星氷の形成条件を調査する.

主な方法:

ヘール・ボップ彗星のソフトX線画像.
X線放射のスペクトル分析.
太陽光の大量と理論モデルとの比較.

主要な成果:

X線放射が検出され,核から中心的な特徴がオフセットされ,粉塵ジェットと相関しない拡張された特徴があります.
ネオンの枯渇は,太陽の豊富さと比較して25倍以上の倍数です.
584アングストームのヘリウム線放射の検出,おそらく太陽風の電荷移転によるものです.
イオン化された酸素とヘリウムに起因する538アングストームの放射の観測.

結論:

ヘイル・ボップの彗星の氷は,おそらく25ケルビン以上の温度で形成された.
太陽風の相互作用は,彗星のX線放射に作用する.
X線観測は,彗星の組成と過程に関するユニークな洞察を提供します.

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