Localized Recombining Plasma in G166.0+4.3: A Supernova Remnant with an Unusual Morphology
Localized Recombining Plasma in G166.0+4.3: A Supernova Remnant with an Unusual Morphology
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DOI：
10.1093/pasj/psx001
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发表时间：
2017-01
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影响因子：
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通讯作者：
Hideaki Matsumura;H. Uchida;Takaaki Tanaka;T. Tsuru;M. Nobukawa;K. Nobukawa;Makoto Itou
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文献类型：
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作者：
Hideaki Matsumura;H. Uchida;Takaaki Tanaka;T. Tsuru;M. Nobukawa;K. Nobukawa;Makoto Itou
我们用朱雀号观测了银河系混合形态超新星遗迹G166.0+4.3。残骸西部的X射线谱由单组分电离等离子体模型很好地表示。东北部地区的光谱可以用两个分量来解释。一个是富Fe组分，其电子温度kT_e = 0.87 - 0.03 ^{+0.02} keV。另一个是轻元素的复合等离子体成分，其能量为kT_e = 0. 46 pm 0. 03 keV，初始温度kT_{init} = 3 keV（固定），电离参数n_et =（6. 1 - 0. 4 ^{+0. 5}）× 10^{11} rm cm^{-3} s。对于复合等离子体的形成过程，考虑了稀薄和热传导两种情况。前者将不被看好，因为我们发现重组血浆只在东北地区，而后者将解释RP的起源。在后一种情况下，预计在爆炸波与冷的致密气体接触的残骸的一部分中会出现RP。排放测量表明东北部地区的环境气体密度较高。射电壳层的形态和GeV的伽马射线发射也表明该区域存在分子云。
We observed the Galactic mixed-morphology supernova remnant G166.0+4.3 with Suzaku. The X-ray spectrum in the western part of the remnant is well represented by a one-component ionizing plasma model. The spectrum in the northeastern region can be explained by two components. One is the Fe-rich component with the electron temperature $kT_e = 0.87_{-0.03}^{+0.02}$ keV. The other is the recombining plasma component of lighter elements with $kT_e = 0.46\pm0.03$ keV, the initial temperature $kT_{init} = 3$ keV (fixed) and the ionization parameter $n_et = (6.1_{-0.4}^{+0.5}) \times 10^{11} \rm cm^{-3} s$. As the formation process of the recombining plasma, two scenarios, the rarefaction and thermal conduction, are considered. The former would not be favored since we found the recombining plasma only in the northeastern region whereas the latter would explain the origin of the RP. In the latter scenario, an RP is anticipated in a part of the remnant where blast waves are in contact with cool dense gas. The emission measure suggests higher ambient gas density in the northeastern region. The morphology of the radio shell and a GeV gamma-ray emission also suggest a molecular cloud in the region.