Dense gas towards the RXJ1713.7-3946 supernova remnant
Dense gas towards the RXJ1713.7-3946 supernova remnant
复制标题
致密气体流向 RXJ1713.7-3946 超新星遗迹
DOI：
10.1063/1.4772245
复制
发表时间：
2012
期刊：
影响因子：
--
通讯作者：
Nigel I.
中科院分区：
文献类型：
--
作者：
Maxted;Nigel I.
我们介绍了Mopra 7 mm波长巡天的结果，该巡天的目标是致密气体示踪CS（1-0）向年轻的γ射线亮超新星遗迹RX J1713.7-3946（SNR G 347.3−0.5）的跃迁。在强子γ射线发射场景中，宇宙射线（CR）质子与气体相互作用产生观测到的γ射线发射，潜在CR靶材料的质量是一个重要因素。我们总结了新发现的致密气体成分，包括核心G和L，以及质量为1 - 104 M Ω的团块N1，N2，N3和T1。我们认为，这些组件是不太可能的贡献显着的γ射线发射的强子γ射线发射的情况。如果RX J1713.7-3946处于目前有利的~1 kpc距离或替代的~6 kpc距离（如以前的一些研究所建议的），情况就是这样。虽然没有观测到与RX J1713.7-3946激波对应的SiO辐射，但振动激发的SiO（1-0）脉泽辐射被发现朝向可能是演化的星星。相隔1年的观测证实了一个短暂的性质，因为SiO（J = 1-0，v = 1，2）发射的强度，线宽和中心速度变化显着。
We present results from a Mopra 7 mm-wavelength survey that targeted the dense gas-tracing CS(1-0) transition towards the young γ-ray-bright supernova remnant, RX J1713.7–3946 (SNR G 347.3−0.5). In a hadronic γ-ray emission scenario, where cosmic ray (CR) protons interact with gas to produce the observed γ-ray emission, the mass of potential CR target material is an important factor. We summarise newly discovered dense gas components, towards Cores G and L, and Clumps N1, N2, N3, and T1, which have masses of 1 – 104 M⊙. We argue that these components are not likely to contribute significantly to γ-ray emission in a hadronic γ-ray emission scenario. This would be the case if RX J1713.7–3946 were at either the currently favoured distance of ~1 kpc or an alternate distance (as suggested in some previous studies) of ~6 kpc.This survey also targeted the shock-tracing SiO molecule. Although no SiO emission corresponding to the RX J1713.7–3946 shock was observed, vibrationally excited SiO(1-0) maser emission was discovered towards what may be an evolved star. Observations taken 1 yr apart confirmed a transient nature, since the intensity, line-width, and central velocity of SiO(J = 1-0,v = 1,2) emission varied significantly.