Erratum: Modelling the ArH+ emission from the Crab Nebula
Erratum: Modelling the ArH+ emission from the Crab Nebula
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勘误表：模拟蟹状星云的 ArH 发射
DOI：
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发表时间：
2017
影响因子：
4.8
通讯作者：
S. Viti
中科院分区：
文献类型：
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作者：
F. Priestley;M. Barlow;S. Viti
我们对中心脉冲星风星云的同步辐射和高通量带电粒子作用下的蟹状星云灯丝进行了光电离和光解离区（PDR）模拟;大大增强的宇宙射线电离率超过标准星际值，zeta_0，需要解释的是，在发表的Herschel SPIRE FTS观测蟹状星云中没有检测到[C I]发射。在SPIRE FTS频率范围内观察到的OH$^+$和ArH$^+$跃迁的线表面亮度比，只能用高宇宙线电离率和较低的ArH$^+$解离复合率来解释，尽管与实验上限一致。我们发现ArH$^+$/OH$^+$谱线强度和观察到的H $2 $振转辐射可以用具有$n_{
m{H}} = 2 x = 10^4$ cm$^{-3}$，$zeta = 10^7 zeta_0$和在蟹状星云中尘埃球的可见光范围内，尽管来自[O I]和[C II]的远红外辐射高于观测限制。具有$n_{
m{H}} = 1900$ cm$^{-3}$低估了H$2 $表面亮度，但与ArH$^+$和OH$^+$表面亮度一致，预测的[O I]和[C II]线比与观测一致。这些模型预测HeH$^+$的旋转发射高于检测阈值，但考虑到形成的时间尺度，蟹状星云中这种分子的丰度应该低于我们分析中获得的平衡值。
We have performed combined photoionization and photodissociation region (PDR) modelling of a Crab Nebula filament subjected to the synchrotron radiation from the central pulsar wind nebula, and to a high flux of charged particles; a greatly enhanced cosmic ray ionization rate over the standard interstellar value, $zeta_0$, is required to account for the lack of detected [C I] emission in published Herschel SPIRE FTS observations of the Crab Nebula. The observed line surface brightness ratios of the OH$^+$ and ArH$^+$ transitions seen in the SPIRE FTS frequency range can only be explained with both a high cosmic ray ionization rate and a reduced ArH$^+$ dissociative recombination rate compared to that used by previous authors, although consistent with experimental upper limits. We find that the ArH$^+$/OH$^+$ line strengths and the observed H$_2$ vibration-rotation emission can be reproduced by model filaments with $n_{
m{H}} = 2 imes 10^4$ cm$^{-3}$, $zeta = 10^7 zeta_0$ and visual extinctions within the range found for dusty globules in the Crab Nebula, although far-infrared emission from [O I] and [C II] is higher than the observational constraints. Models with $n_{
m{H}} = 1900$ cm$^{-3}$ underpredict the H$_2$ surface brightness, but agree with the ArH$^+$ and OH$^+$ surface brightnesses and predict [O I] and [C II] line ratios consistent with observations. These models predict HeH$^+$ rotational emission above detection thresholds, but consideration of the formation timescale suggests that the abundance of this molecule in the Crab Nebula should be lower than the equilibrium values obtained in our analysis.
影响因子：
6.5
作者：
Schilke, P.;Neufeld, D. A.;Falgarone, E.
通讯作者：
Falgarone, E.