THE ORIGIN OF THE IRON-RICH KNOT IN TYCHO’S SUPERNOVA REMNANT
THE ORIGIN OF THE IRON-RICH KNOT IN TYCHO’S SUPERNOVA REMNANT
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第谷超新星遗迹中富铁结的起源
DOI：
10.3847/1538-4357/834/2/124
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发表时间：
2016
期刊：
影响因子：
--
通讯作者：
R. Petre
中科院分区：
文献类型：
--
作者：
H. Yamaguchi;J. Hughes;C. Badenes;E. Bravo;I. Seitenzahl;H. Martínez;Sangwook Park;R. Petre
超新星遗迹（SNRs）的X射线观测使我们能够研究喷出物的化学不均匀性，为超新星爆炸中的核合成提供独特的见解。在这里，我们提出了详细的成像和光谱研究的“铁结”位于沿着东部边缘的Ia型信噪比第谷（SN 1572）使用朱雀和钱德拉长曝光数据。令人惊讶的是，这个结的朱雀光谱显示没有来自Cr，Mn或Ni的发射，这对于这个SNR中的富铁区域是不寻常的。在超新星Ia的典型延迟爆轰模型框架内，观测到的质量比，和（90%置信度）只能在峰值温度为（5.3-5.7）K和中子过剩为。这些限制排除了铁结起源于一颗质量为1000亿克拉塞卡的白色矮星的深而致密的核心，而有利于不完全的硅燃烧或富含α的冻结状态，可能靠近边界。一个爆炸性的他燃烧制度是一个可能的替代方案，虽然这一假设是在冲突的主要属性，这SNR。
X-ray observations of supernova remnants (SNRs) allow us to investigate the chemical inhomogeneity of ejecta, offering unique insight into the nucleosynthesis in supernova explosions. Here we present detailed imaging and spectroscopic studies of the “Fe knot” located along the eastern rim of the Type Ia SNR Tycho (SN 1572) using Suzaku and Chandra long-exposure data. Surprisingly, the Suzaku spectrum of this knot shows no emission from Cr, Mn, or Ni, which is unusual for the Fe-rich regions in this SNR. Within the framework of the canonical delayed-detonation models for SN Ia, the observed mass ratios , , and (at 90% confidence) can only be achieved for a peak temperature of (5.3–5.7) K and a neutron excess of . These constraints rule out the deep, dense core of a Chandrasekhar-mass white dwarf as the origin of the Fe knot and favor either incomplete Si burning or an α-rich freeze-out regime, probably close to the boundary. An explosive He burning regime is a possible alternative, although this hypothesis is in conflict with the main properties of this SNR.
影响因子：
4.8
作者：
I. Seitenzahl;F. Ciaraldi-Schoolmann;F. Roepke;M. Fink;W. Hillebrandt;M. Kromer;R. Pakmor;A. Ruiter-A
通讯作者：
I. Seitenzahl;F. Ciaraldi-Schoolmann;F. Roepke;M. Fink;W. Hillebrandt;M. Kromer;R. Pakmor;A. Ruiter-A