新德尔菲尼2013年扩大的火球
G H Schaefer1, T ten Brummelaar1, D R Gies2
1The CHARA Array of Georgia State University, Mount Wilson Observatory, Mount Wilson, California 91023, USA.
Nature
|November 4, 2014
概括
早期对2013年诺瓦·德尔菲尼的观测揭示了其结构,使用近红外干扰测量. 这项研究表明,在白矮星上的热核失控之后,双极形状迅速发展.
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:
- 经典的新星是由于热核在二进制星系中的白矮星上积累的失控.
- 晚期喷射结构可能来自共同包膜相互作用或内在双极爆炸.
- 由于需要高空间分辨率,早期新星结构研究很困难.
研究的目的:
- 调查2013年诺瓦·德尔菲尼早期结构和扩张.
- 用它的角度膨胀和辐射速度来确定距离Nova Delphini 2013的距离.
主要方法:
- 接近红外的干扰度测量Nova Delphini 2013的角度尺寸,从爆炸后的一天开始.
- 在前43天持续监测以追踪明显扩张率的变化.
- 结合角度膨胀数据与辐射速度测量以确定距离.
主要成果:
- 观察到的膨胀速率变化与光学上厚厚的核心和扩散外模型相一致.
- 检测到光分布的圆性,表明在第二天前前进或双极结构.
- 一个几何距离为4.54±0.59千帕塞克的Nova Delphini 2013的导出.
结论:
- 2013年诺瓦·德尔菲尼在其演变的早期呈现出双极结构.
- 膨胀的喷射物随着分散而变化的光学深度.
- 导出的距离为理解这个经典的新星事件提供了一个关键参数.
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