用银心磁Turbulence加速Cosmic-Ray的可行性评估
Assessing the Feasibility of Cosmic-Ray Acceleration by Magnetic Turbulence at the Galactic Center
摘要：
银河系中心存在相对论粒子的证据是从银河系内部$\sim$ $2^\circ$探测到的弥散TeV辐射。虽然还不完全清楚TeV光子的起源是由于强子相互作用还是轻子相互作用，但强度分布与沿银河山脊的分子气体分布的紧密相关性强烈地指向涉及相对论质子的π衰变过程。在早期的工作中，我们得出的结论是，点源候选者，如超大质量黑洞人马座A*（与HESS源J1745-290确定），或脉冲星风星云沿银河平面分散，不能解释观察到的弥漫TeV辐射从这个地区。受此结果的启发，我们认为在这里的可行性，宇宙射线填充的银河系中心（GC）地区的磁湍流加速原位。我们的研究结果表明，即使在一个高导电性的环境中，这种机制是足够有效的激励质子内的intercloud介质的$\ga $ TeV的能量需要产生的HESS发射。
英文摘要：
The presence of relativistic particles at the center of our galaxy is evidenced by the diffuse TeV emission detected from the inner $\sim$$2^\circ$ of the Galaxy. Although it is not yet entirely clear whether the origin of the TeV photons is due to hadronic or leptonic interactions, the tight correlation of the intensity distribution with the distribution of molecular gas along the Galactic ridge strongly points to a pionic-decay process involving relativistic protons. In earlier work, we concluded that point-source candidates, such as the supermassive black hole Sagittarius A* (identified with the HESS source J1745-290), or the pulsar wind nebulae dispersed along the Galactic plane, could not account for the observed diffuse TeV emission from this region. Motivated by this result, we consider here the feasibility that the cosmic rays populating the Galactic Center (GC) region are accelerated in situ by magnetic turbulence. Our results indicate that even in a highly conductive environment, this mechanism is efficient enough to energize protons within the intercloud medium to the $\ga $ TeV energies required to produce the HESS emission.
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