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巨大な星. 巨大な星. 第一世代の非常に巨大な恒星の化学的シグネチャー

W Aoki¹, N Tominaga², T C Beers³

¹National Astronomical Observatory of Japan (NAOJ), 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan. Department of Astronomical Science, School of Physical Sciences, The Graduate University for Advanced Studies (SOKENDAI), 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan. aoki.wako@nao.ac.jp.

Science (New York, N.Y.)

|August 23, 2014

まとめ

研究者たちは,金属が少ない星,SDSS J001820.5-093939.2を分析し,ユニークな元素の豊富さを発見しました. これらのパターンは,非常に巨大な恒星の超新星から形成されたことを示唆しています,潜在的に100太陽質量以上です.

科学分野:

天文学と天体物理学について
コスモロジー・コスモロジーとは
恒星の進化について

背景:

初期の宇宙のシミュレーションでは,巨大な恒星 (太陽の質量数百個) が予測されています.
これらの非常に巨大な恒星からの超新星は,天の川銀河の星組成でははっきりと検出されません.
最初の星の核合成産物に対する観測的証拠は,初期の宇宙の化学的濃縮を理解するために極めて重要です.

研究の目的:

特殊な金属が少ない星,SDSS J001820.5-093939.2.2.の化学組成を調査する.
恒星の元素の豊富さが,非常に巨大な第一世代の恒星からの超新星に関する予測と一致するかどうかを判断するために.
初期の宇宙における星の質量分布を制限するために.

主な方法:

SDSS J001820.5-093939.2.2.のスペクトルにおける元素豊富度比の分析について
観測された豊富さの比較と,超大質量星の超新星に対する理論的な核合成モデル.
低い[α-元素/Fe]比と大きな奇数対数元素の多量対比の特徴.

主要な成果:

恒星SDSS J001820.5-093939.2は,元素の豊富度比がユニークであることを示しています.
観測された豊富さは,低い[α-元素/Fe]比を示し,奇数と偶数元素のペア (例えば,Sc/Ti,Co/Ni) の間の大きなコントラストを示しています.
これらの特徴は,140太陽質量を超える恒星からの超新星に関する予測と一致しています.

結論:

SDSS J001820.5-093939.2の化学的サインは,非常に大きな恒星からの超新星の存在の証拠を提供します.
この発見は,第一世代の恒星の質量分布が,太陽の質量100倍以上まで広がる可能性があることを示唆している.
この研究は,最も初期の恒星のほとんど理解されていない核合成への潜在的観測的リンクを提供します.

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