ヘリウム不透明性の変化による輝く青色の変数星の爆発
Yan-Fei Jiang1, Matteo Cantiello2,3, Lars Bildsten4,5
1Kavli Institute for Theoretical Physics, University of California, Santa Barbara, CA, USA. yanfei@kitp.ucsb.edu.
Nature
|September 28, 2018
まとめ
3Dシミュレーションで示されたように,巨大な明るい青色の変数星は,ヘリウム不透明性のために爆発を経験します. これらのシミュレーションは,恒星の半径と明るさの短期的な変動も予測します.
科学分野:
- 天文学と天体物理学
- スター進化
- 計算による天体物理学
背景:
- 輝く青色変数 (LBV) は巨大で進化した星で,輝度や大きさの大きな変化があることが知られている.
- これらの恒星は高質量損失率を示し,爆発段階を経て,実際の温度を下げます.
- LBV爆発の背後にある物理的メカニズムを説明するには,現在の一次元モデルは不十分です.
研究 の 目的:
- 物理的なメカニズムを調査するために 爆発と質量損失を駆動する 巨大な放射線が支配する星.
- 恒星の変動におけるヘリウム不透明性とコンベクションの役割を調査する.
- LBVの行動を理解するためのより正確なモデルを開発する.
主な方法:
- 巨大で放射線が支配する星の 3次元水力学シミュレーション
- 恒星の密度と温度をコンベクションで自律的に測定する.
- 恒星の構造と動態に対するヘリウム不透明性の影響をモデル化.
主要な成果:
- ヘリウム不透明性は LBVの爆発を誘発し 効果温度を9000ケルビンに設定する上で 重要な役割を果たします
- シミュレーションでは,年に10^-7から10^-5の太陽質量の割合でエピソード的な質量損失を示しています.
- 三次元モデルでは,恒星半径におけるコンベクションによる不規則な振動と,短い時間スケールの10-30%の明るさの変動が示されています.
結論:
- 立体シミュレーションは LBV 爆発に関する新しい洞察を提供し,ヘリウム不透明性の重要性を強調しています.
- コンベクションは恒星の変動に大きく影響し,観測可能な短時間の振動につながります.
- これらの発見は,正確な天体物理学的な予測のために,一次元,球面対称的なアプローチを超えた高度なモデリングを必要とします.
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