Solar Energetic Particle Events Observed by the PAMELA Mission
Solar Energetic Particle Events Observed by the PAMELA Mission
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DOI：
10.3847/1538-4357/aacc26
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发表时间：
2018-07
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通讯作者：
A. Bruno;G. Bazilevskaya;M. Boezio;E. Christian;G. Nolfo;M. Martucci;M. Mergé;V. Mikhailov;R. Munini;Ian G. Richardson;Ian G. Richardson;James Ryan;S. Stochaj;O. Adriani;G. Barbarino;R. Bellotti;É. Bogomolov;M. Bongi;V. Bonvicini;S. Bottai;F. Cafagna;D. Campana;P. Carlson;M. Casolino;G. Castellini;C. Santis;V. Felice;A. Galper;A. Karelin;S. Koldashov;S. Koldobskiy;S. Krutkov;A. Kvashnin;A. Leonov;V. Malakhov;L. Marcelli;A. Mayorov;W. Menn;E. Mocchiutti;A. Monaco;N. Mori;G. Osteria;B. Panico;P. Papini;M. Pearce;P. Picozza;M. Ricci;S. Ricciarini;M. Simon;R. Sparvoli;P. Spillantini;P. Spillantini;Y. Stozhkov;A. Vacchi;E. Vannuccini;G. Vasilyev;S. Voronov;Y. Yurkin;G. Zampa;N. Zampa
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作者：
A. Bruno;G. Bazilevskaya;M. Boezio;E. Christian;G. Nolfo;M. Martucci;M. Mergé;V. Mikhailov;R. Munini;Ian G. Richardson;Ian G. Richardson;James Ryan;S. Stochaj;O. Adriani;G. Barbarino;R. Bellotti;É. Bogomolov;M. Bongi;V. Bonvicini;S. Bottai;F. Cafagna;D. Campana;P. Carlson;M. Casolino;G. Castellini;C. Santis;V. Felice;A. Galper;A. Karelin;S. Koldashov;S. Koldobskiy;S. Krutkov;A. Kvashnin;A. Leonov;V. Malakhov;L. Marcelli;A. Mayorov;W. Menn;E. Mocchiutti;A. Monaco;N. Mori;G. Osteria;B. Panico;P. Papini;M. Pearce;P. Picozza;M. Ricci;S. Ricciarini;M. Simon;R. Sparvoli;P. Spillantini;P. Spillantini;Y. Stozhkov;A. Vacchi;E. Vannuccini;G. Vasilyev;S. Voronov;Y. Yurkin;G. Zampa;N. Zampa
尽管近年来取得了重大进展，但太阳高能粒子（SEP）起源的物理机制仍然是一个争论的问题。粒子加速和传输的复杂性质对开发SEP事件的通用图像提出了挑战，该图像包括天基仪器进行的低能（从几十keV到几百MeV）观测和全球中子监测器网络在地面增强（GLE）中检测到的GeV粒子。反物质探测和轻核天体物理学卫星实验有效载荷收集的高精度数据为研究1080 MeV至几GeV之间的SEP通量提供了一个独特的机会，大大改善了对最具活力事件的定性。特别是，PAMELA可以测量第一次在中等和高能量的光谱特征，提供了重要的限制，目前SEP模型具有良好的精度。此外，PAMELA观测允许研究低能和高能粒子之间的关系，从而能够更清楚地了解SEP的起源。GLE，子GLE和非GLE事件的光谱形状之间没有定性的区别，这表明GLE不是一个单独的类，而是SEP事件的连续分布的子集，在高能量下更强烈。虽然发现的光谱形式是一致的扩散冲击加速理论，该理论预测在高能量的频谱翻转，这是由于粒子逃逸的冲击区在加速过程中，需要进一步的工作，以探索加速和运输过程对SEP谱的相对影响。
Despite the significant progress achieved in recent years, the physical mechanisms underlying the origin of solar energetic particles (SEPs) are still a matter of debate. The complex nature of both particle acceleration and transport poses challenges to developing a universal picture of SEP events that encompasses both the low-energy (from tens of keV to a few hundreds of MeV) observations made by space-based instruments and the GeV particles detected by the worldwide network of neutron monitors in ground-level enhancements (GLEs). The high-precision data collected by the Payload for Antimatter Matter Exploration and Light-nuclei Astrophysics (PAMELA) satellite experiment offer a unique opportunity to study the SEP fluxes between ∼80 MeV and a few GeV, significantly improving the characterization of the most energetic events. In particular, PAMELA can measure for the first time with good accuracy the spectral features at moderate and high energies, providing important constraints for current SEP models. In addition, the PAMELA observations allow the relationship between low- and high-energy particles to be investigated, enabling a clearer view of the SEP origin. No qualitative distinction between the spectral shapes of GLE, sub-GLE and non-GLE events is observed, suggesting that GLEs are not a separate class, but are the subset of a continuous distribution of SEP events that are more intense at high energies. While the spectral forms found are to be consistent with diffusive shock acceleration theory, which predicts spectral rollovers at high energies that are attributed to particles escaping the shock region during acceleration, further work is required to explore the relative influences of acceleration and transport processes on SEP spectra.