Evidence of Energy and Charge Sign Dependence of the Recovery Time for the 2006 December Forbush Event Measured by the PAMELA Experiment
Evidence of Energy and Charge Sign Dependence of the Recovery Time for the 2006 December Forbush Event Measured by the PAMELA Experiment
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DOI：
10.3847/1538-4357/aaa0c8
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发表时间：
2018-01
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通讯作者：
R. Munini;M. Boezio;A. Bruno;E. Christian;G. Nolfo;V. Felice;M. Martucci;M. Mergé;I. Richardson;I. Richardson;J. Ryan;S. Stochaj;O. Adriani;G. Barbarino;G. Bazilevskaya;R. Bellotti;M. Bongi;V. Bonvicini;S. Bottai;F. Cafagna;D. Campana;P. Carlson;M. Casolino;G. Castellini;C. Santis;A. Galper;A. Karelin;S. Koldashov;S. Koldobskiy;S. Krutkov;A. Kvashnin;A. Leonov;V. Malakhov;L. Marcelli;A. Mayorov;W. Menn;V. Mikhailov;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;Y. Stozhkov;A. Vacchi;E. Vannuccini;G. Vasilyev;S. Voronov;Y. Yurkin;G. Zampa;N. Zampa;M. Potgieter
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作者：
R. Munini;M. Boezio;A. Bruno;E. Christian;G. Nolfo;V. Felice;M. Martucci;M. Mergé;I. Richardson;I. Richardson;J. Ryan;S. Stochaj;O. Adriani;G. Barbarino;G. Bazilevskaya;R. Bellotti;M. Bongi;V. Bonvicini;S. Bottai;F. Cafagna;D. Campana;P. Carlson;M. Casolino;G. Castellini;C. Santis;A. Galper;A. Karelin;S. Koldashov;S. Koldobskiy;S. Krutkov;A. Kvashnin;A. Leonov;V. Malakhov;L. Marcelli;A. Mayorov;W. Menn;V. Mikhailov;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;Y. Stozhkov;A. Vacchi;E. Vannuccini;G. Vasilyev;S. Voronov;Y. Yurkin;G. Zampa;N. Zampa;M. Potgieter
介绍了PAMELA仪器测量的2006年12月短期银河宇宙线（GCR）强度变化（Forbish下降）的新结果。Forbush衰减是GCR强度的突然增强，它与行星际瞬变（如激波和行星际日冕物质抛射（ICME））的通过有关。过去对这种现象的大多数测量都是用地基探测器进行的，如中子监测器或μ子望远镜。这些技术仅允许在积分能量范围内间接检测总体GCR强度。由于PAMELA磁谱仪的独特功能，首次在宽刚度范围（0.4-20 GV）和直接在空间检测到的不同种类的GCR中研究了福布什减少，从2006年12月14日开始，并在2006年12月13日在太阳进行CME之后。利用日平均GCR质子强度研究了Forbush下降幅度和恢复时间的刚性依赖性。此外，首次研究了在福布什减少过程中氦和电子强度的时间变化。有趣的是，氦和质子强度的时间演变过程中的福布什减少被发现是在良好的协议，而低刚性电子（GV）显示出更快的恢复。电子恢复的这种差异被解释为电荷符号依赖性所经历的GCR在其传播过程中通过日光层的漂移运动。
New results on the short-term galactic cosmic-ray (GCR) intensity variation (Forbish decrease) in 2006 December measured by the PAMELA instrument are presented. Forbush decreases are sudden suppressions of the GCR intensities, which are associated with the passage of interplanetary transients such as shocks and interplanetary coronal mass ejections (ICMEs). Most of the past measurements of this phenomenon were carried out with ground-based detectors such as neutron monitors or muon telescopes. These techniques allow only the indirect detection of the overall GCR intensity over an integrated energy range. For the first time, thanks to the unique features of the PAMELA magnetic spectrometer, the Forbush decrease, commencing on 2006 December 14 and following a CME at the Sun on 2006 December 13, was studied in a wide rigidity range (0.4–20 GV) and for different species of GCRs detected directly in space. The daily averaged GCR proton intensity was used to investigate the rigidity dependence of the amplitude and the recovery time of the Forbush decrease. Additionally, for the first time, the temporal variations in the helium and electron intensities during a Forbush decrease were studied. Interestingly, the temporal evolutions of the helium and proton intensities during the Forbush decrease were found to be in good agreement, while the low rigidity electrons ( GV) displayed a faster recovery. This difference in the electron recovery is interpreted as a charge sign dependence introduced by drift motions experienced by the GCRs during their propagation through the heliosphere.