来自相对论耀斑电子和正电子的逆康普顿X射线
Inverse Compton X-rays from relativistic flare electrons and positrons
摘要：
在太阳耀斑中，光球光子的逆康普顿散射（ICS）可能会引起来自日冕的可检测的硬X射线光子通量，其中环境密度太低，无法进行显着的韧致辐射或复合。在一些大耀斑中的伽马射线线和连续谱意味着存在必要的~100 MeV电子和正电子，后者是GeV能量离子的副产品。最近对日冕硬X射线源的观测特别促使我们重新考虑ICS的可能贡献。我们的目标是评估ICS的X射线通量预计从规定的相对论性电子和正电子在日冕的人口。最终的目的是确定ICS日冕X射线源是否可以提供一个新的诊断窗口相对论电子和离子的耀斑。我们使用完整的形式主义的ICS计算X射线通量从耀斑的初级电子和次级正电子的可能的人口，注意入射光子的角分布附近的太阳表面，从而提高在以前的太阳讨论的各向同性的假设。初级电子和次级正电子都产生非常硬的ICS X射线谱。各向异性的初级辐射场的结果在预测的通量和光谱，最强烈的光谱，延伸到最高的光子能量，预计从临边耀斑的中心到临边的变化。可接受的电子或正电子数量可以解释RHESSI日冕X/伽马射线源。某些日冕X射线源至少可以用相对论电子或正电子的ICS来解释，特别是当源出现在如此低的环境密度下时，韧致辐射似乎是不可信的。
英文摘要：
In solar flares, inverse Compton scattering (ICS) of photospheric photons might give rise to detectable hard X-ray photon fluxes from the corona where ambient densities are too low for significant bremsstrahlung or recombination. Gamma-ray lines and continuum in some large flares imply the presence of the necessary ~100 MeV electrons and positrons, the latter as by-products of GeV energy ions. Recent observations of coronal hard X-ray sources in particular prompt us to reconsider here the possible contribution of ICS. We aim to evaluate the ICS X-ray fluxes to be expected from prescribed populations of relativistic electrons and positrons in the solar corona. The ultimate aim is to determine if ICS coronal X-ray sources might offer a new diagnostic window on relativistic electrons and ions in flares. We use the complete formalism of ICS to calculate X-ray fluxes from possible populations of flare primary electrons and secondary positrons, paying attention to the incident photon angular distribution near the solar surface and thus improving on the assumption of isotropy made in previous solar discussions. Both primary electrons and secondary positrons produce very hard ICS X-ray spectra. The anisotropic primary radiation field results in pronounced centre-to-limb variation in predicted fluxes and spectra, with the most intense spectra, extending to the highest photon energies, expected from limb flares. Acceptable numbers of electrons or positrons could account for RHESSI coronal X/gamma-ray sources. Some coronal X-ray sources at least might be interpreted in terms of ICS by relativistic electrons or positrons, particularly when sources appear at such low ambient densities that bremsstrahlung appears implausible.
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