The Radial Structure of Supernova Remnant N103B
The Radial Structure of Supernova Remnant N103B
复制标题
超新星遗迹N103B的径向结构
DOI：
10.1086/344717
复制
发表时间：
2002
期刊：
影响因子：
--
通讯作者：
J. Nousek
中科院分区：
文献类型：
--
作者：
K. Lewis;D. Burrows;J. Hughes;P. Slane;G. Garmire;J. Nousek
我们报告的结果，从钱德拉ACIS观测的年轻，紧凑，超新星遗迹N103 B。钱德拉前所未有的空间分辨率揭示了亚弧秒结构，无论是在亮度和光谱变化。在这些小尺度变化的基础上，强Si和S发射线的等效宽度中有一个令人惊讶的简单径向结构。我们调查这些径向变化，通过空间分辨光谱，使用平面平行，非平衡电离模型与多个组件。大部分发射来自温度为1 keV的组分：完全电离的氢组分;含有Si、S、Ar、Ca和Fe的高电离时间尺度（净> 1012 s cm-3）组分;以及低电离时间尺度（净~ 1011 s cm-3）的O、Ne和Mg组分。为了再现强Fe Kα线，有必要在热（> 2 keV）、低电离时间尺度（净~ 1010.8 s cm-3）分量中包含额外的Fe。这种热铁可能是以热铁泡的形式存在，是在56镍块的放射性衰变中形成的。我们发现没有径向变化的电离时间尺度或温度的各种组件。相反，Si和S的等效宽度在大半径处增加，因为这些线以及Ar和Ca的线形成于占据残余物外半部的壳层中。一个热铁壳层位于其内部，但这两个壳层之间有很大的重叠区域。在内部30%的残余物中，有一个较冷的核心，1 keV的Fe。我们发现，喷出物的分布和产量的中间质量的物种是一致的模式预测Ia型事件。
We report on the results from a Chandra ACIS observation of the young, compact, supernova remnant N103B. The unprecedented spatial resolution of Chandra reveals subarcsecond structure, in both the brightness and spectral variations. Underlying these small-scale variations is a surprisingly simple radial structure in the equivalent widths of the strong Si and S emission lines. We investigate these radial variations through spatially resolved spectroscopy, using a plane-parallel, nonequilibrium ionization model with multiple components. The majority of the emission arises from components with a temperature of 1 keV: a fully ionized hydrogen component; a high ionization timescale (net > 1012 s cm-3) component containing Si, S, Ar, Ca, and Fe; and a low ionization timescale (net ~ 1011 s cm-3) O, Ne, and Mg component. To reproduce the strong Fe Kα line, it is necessary to include additional Fe in a hot (> 2 keV), low ionization timescale (net ~ 1010.8 s cm-3) component. This hot Fe might be in the form of hot Fe bubbles, formed in the radioactive decay of clumps of 56Ni. We find no radial variation in the ionization timescales or temperatures of the various components. Rather, the Si and S equivalent widths increase at large radii because these lines, as well as those of Ar and Ca, are formed in a shell occupying the outer half of the remnant. A shell of hot Fe is located interior to this, but there is a large region of overlap between these two shells. In the inner 30% of the remnant, there is a core of cooler, 1 keV Fe. We find that the distribution of the ejecta and the yields of the intermediate-mass species are consistent with model prediction for Type Ia events.