论文标题
大型麦哲伦云超新星残留N132D的空间分辨的钱德拉光谱
Spatially Resolved Chandra Spectroscopy of the Large Magellanic Cloud Supernova Remnant N132D
论文作者
论文摘要
我们使用Chandra Archival观测值对大麦芽云（LMC）（LMC）中的X射线最亮的超新星残留（SNR）进行详细的光谱。通过分析整个定义明确的边缘的光谱，我们确定局部LMC环境中O，NE，MG，SI，S和FE的平均丰度。我们发现西北爆炸波的西北和s的O增强的证据。通过分析残留物的光谱，我们确认存在富含Si的相对热等离子体（> 1.5 KEV），该血浆也是Fe K发射的原因。 Chandra图像显示，Fe K发射分布在整个残留的南部的内部，但不会扩展到爆炸波。我们使用丰度比在不同地区估计祖细胞质量为$ 15 \ pm5 \，m _ {\ odot} $，与恒星风中造成的空腔中的爆炸模型相比，在不同区域以及从远期冲击的半径中，这些区域集体覆盖了很大一部分。我们将离子化和重新组合的等离子体模型拟合到Fe K发射，发现当前数据无法区分两者，因此高温等离子体的起源仍然不确定。我们的分析与N132D是由其中间质量祖细胞产生的腔中核心折叠超新星的结果。
We perform detailed spectroscopy of the X-ray brightest supernova remnant (SNR) in the Large Magellanic Cloud (LMC), N132D, using Chandra archival observations. By analyzing the spectra of the entire well-defined rim, we determine the mean abundances for O, Ne, Mg, Si, S and Fe for the local LMC environment. We find evidence of enhanced O on the north-western and S on the north-eastern blast wave. By analyzing spectra interior to the remnant, we confirm the presence of a Si-rich relatively hot plasma (> 1.5 kev) that is also responsible for the Fe K emission. Chandra images show that the Fe K emission is distributed throughout the interior of the southern half of the remnant but does not extend out to the blast wave. We estimate the progenitor mass to be $15\pm5\,M_{\odot}$ using abundance ratios in different regions that collectively cover a large fraction of the remnant, as well as from the radius of the forward shock compared with models of an explosion in a cavity created by stellar winds. We fit ionizing and recombining plasma models to the Fe K emission and find that the current data cannot distinguish between the two, hence the origin of the high-temperature plasma remains uncertain. Our analysis is consistent with N132D being the result of a core-collapse supernova in a cavity created by its intermediate mass progenitor.
