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脉冲对的不稳定性是对最亮的超新星的解释
S E Woosley1, S Blinnikov, Alexander Heger
1Department of Astronomy and Astrophysics, UCSC, Santa Cruz, California 95064, USA. woosley@ucolick.org
Nature
|November 16, 2007
概括
明亮的超新星是来自巨大的恒星撞击的弹射的结果,这些巨大的恒星经历了对不稳定. 这个过程解释了像SN 2006gy这样的极度亮度事件,挑战了核心崩模型.
科学领域:
- 天文学 天文学
- 天体物理学 天体物理学
- 恒星进化 恒星进化
背景情况:
- 超新星对于理解恒星进化和宇宙学至关重要.
- 超新星SN 2006gy的极端亮度挑战了传统的恒星核心崩模型.
- 据认为,大质量恒星以超新星的形式结束了他们的生命.
研究的目的:
- 为了解释极其明亮的超新星的起源,如SN 2006gy.
- 为巨大的恒星中超新星爆炸提出一种替代机制.
- 为了建模对不稳定的超新星的光曲线.
主要方法:
- 开发了由对不稳定驱动的恒星爆炸的理论模型.
- 模拟恒星外的弹射和随后的弹射外的碰撞.
- 将模型预测与观测数据进行比较,特别是SN 2006gy.的光曲线.
主要成果:
- 经历对不稳定的大质量恒星可以弹出多个物质外.
- 这些弹出的外之间的碰撞可以产生比普通超新星大约十倍的亮度.
- 该模型成功地复制了SN 2006gy.gy.观测到的光曲线.
结论:
- 大质量恒星中的对不稳定性为产生极其发光的超新星提供了可行的机制.
- 这种机制挑战了对超新星形成的核心崩的单一依赖.
- 一些大质量恒星在整个进化过程中可能会产生多次超新星般的爆发.
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