銀河の端にあるを含有分子 PO と PN
L A Koelemay1, K R Gold1, L M Ziurys2,3
1Department of Chemistry, University of Arizona, Tucson, AZ, USA.
Nature
|November 8, 2023
まとめ
科学者はPOとPNの分子を用いて外銀河のガス相リンを検出しました この発見は 超新星ではなく アシンプトティックな巨大な分岐星から リンが生まれていることを示唆し 銀河の化学的進化モデルに 挑戦しています
科学分野:
- 天文学と天体物理学
- 天体化学
- 銀河の化学的進化
背景:
- リンは惑星の形成と生物学にとって不可欠ですが 以前は銀河系内側だけに見られていました
- 不利な原子移行により,リンの研究は困難である.
- 銀河の化学的進化の現在のモデルは,観測されたの量に匹敵する超新星生成の恣意的な増加を必要とします.
研究 の 目的:
- 外の銀河でガス相のリンを検出する
- 銀河系におけるの起源と分布を調査する
- 銀河の化学的進化のモデルを改良する
主な方法:
- 一酸化リン (PO) と二酸化リン (PN) のミリメートルスペクトルの観測
- 銀河の中心から22.6キロメートル離れた密集した雲WB89-621の観測.
- POとPNの回転線を分析して,多量性を決定する.
主要な成果:
- 外の銀河で初めてガス相のが検出されました
- 観測されたPOとPNの豊富さは,太陽系に近いものと比較できます.
- 超新星が存在しない外側の銀河にリンが存在することは 代替生産源を示しています
結論:
- 外側の銀河のは,質量が低いアシンプトティック・ジャイアント・ブランチ (AGB) の恒星における中性子捕獲プロセスによって生成される可能性が高い.
- 炭素を産生するAGBの星は,炭素を含む分子と外側の銀河の平らな金属性グラデーションの観測された高い豊富さを説明することができます.
- この発見は,の生産と分布に関する銀河化学進化のモデルを改訂する必要があります.
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