论文标题
Kepler Supernova Remnant中西南Fe富集结构的核合成起源
A Nucleosynthetic Origin for the Southwestern Fe-rich Structure in Kepler's Supernova Remnant
论文作者
论文摘要
{\ it chandra}对开普勒超新星残留物的X射线观测表明，西南地区存在高速富含铁的弹射结构。我们报告了Fe-peak元素（CR，MN，FE，NI）以及CA的强劲K壳发射，在这种富含Fe的结构中，这意味着这些元素可以在爆炸的白矮人的内部区域产生。我们发现CA/FE，Cr/Fe，Mn/Fe和Ni/Fe质量比分别为1.0--4.1 \％，1.0---4.6 \％，1---11 \％和2--30 \％。为了限制可能产生这种结构的燃烧状态，我们将这些观察到的质量比与18个一维IA型核合成模型中的质量比进行了比较（包括接近 - $ M _ {\ rm ch} $和sub- $ m _ {\ rm ch} $爆炸模型）。观察到的质量比与IA类型核合成模型中不完整的SI燃烧中间层的质量比非常吻合，其峰值温度为$ \ sim $（5.0--5.3）$（5.0--5.3）$ \ times $ 10 $^{9} $ k和高金属性，Z $> $ 0.0225。根据我们的结果，我们推断出某种机制产生突出的Fe富含Fe的团块的必要性，该团块在爆炸过程中以不完整的Si燃烧产物为主。我们还讨论了其他类型的IA Supernova残留物中X射线X射线观察的未来观点。
{\it Chandra} X-ray observations of Kepler's supernova remnant indicate the existence of a high speed Fe-rich ejecta structure in the southwestern region. We report strong K-shell emission from Fe-peak elements (Cr, Mn, Fe, Ni), as well as Ca, in this Fe-rich structure, implying that those elements could be produced in the inner area of the exploding white dwarf. We found Ca/Fe, Cr/Fe, Mn/Fe and Ni/Fe mass ratios of 1.0--4.1\%, 1.0--4.6\%, 1--11\% and 2--30\%, respectively. In order to constrain the burning regime that could produce this structure, we compared these observed mass ratios with those in 18 one-dimensional Type Ia nucleosynthesis models (including both near-$M_{\rm Ch}$ and sub-$M_{\rm Ch}$ explosion models). The observed mass ratios agree well with those around the middle layer of incomplete Si-burning in Type Ia nucleosynthesis models with a peak temperature of $\sim$(5.0--5.3)$\times$10$^{9}$ K and a high metallicity, Z $>$ 0.0225. Based on our results, we infer the necessity for some mechanism to produce protruding Fe-rich clumps dominated by incomplete Si-burning products during the explosion. We also discuss the future perspectives of X-ray observations of Fe-rich structures in other Type Ia supernova remnants.
