仙后座A的核退激发线光谱
Nuclear de-excitation line spectrum of Cassiopeia A
摘要：
超新星遗迹仙后座A是加速宇宙射线质子和离子的主要候选者。在GeV和TeV的能量下已经观察到伽马射线，这表明强子相互作用，但它们也可能是由加速电子对低能光子的逆康普顿散射引起的。我们试图预测从Cas A通过低能宇宙射线的核去激发线的通量，并将其与COMPTEL测量进行比较。假设一个强子起源的高能发射，我们外推宇宙射线谱的能量为10兆电子伏，考虑到一个平衡的幂律动量谱与恒定的斜率。然后，我们计算仙后座A的核线光谱，考虑到最突出的化学元素在兆电子伏波段和它们的丰度由X射线光谱测定。我们表明，预测的线光谱是接近的COMPTEL灵敏度的水平，并同意保守的上限。
英文摘要：
The supernova remnant Cassiopeia A is a prime candidate for accelerating cosmic ray protons and ions. Gamma rays have been observed at GeV and TeV energies, which indicates hadronic interactions, but they could also be caused by inverse-Compton scattering of low-energy photons by accelerated electrons. We seek to predict the flux of nuclear de-excitation lines from Cas A through lower-energy cosmic rays and to compare it with COMPTEL measurements. Assuming a hadronic origin of the high-energy emission, we extrapolate the cosmic ray spectrum down to energies of 10 MeV, taking into account an equilibrium power-law momentum spectrum with a constant slope. We then calculate the nuclear line spectrum of Cassiopeia A, considering the most prominent chemical elements in the MeV band and their abundances as determined by X-ray spectroscopy. We show that the predicted line spectrum is close to the level of the COMPTEL sensitivity and agrees with conservative upper limits.
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