2006年7月至2009年12月之间通过Pamela实验测量的宇宙射线中氦核的通量的时间依赖性

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2006年7月至2009年12月之间通过Pamela实验测量的宇宙射线中氦核的通量的时间依赖性

Time dependence of the flux of helium nuclei in cosmic rays measured by the PAMELA experiment between July 2006 and December 2009

论文作者

Marcelli, N., Boezio, M., Lenni, A., Menn, W., Munini, R., Aslam, O. P. M., Bisschoff, D., Ngobeni, M. D., Potgieter, M. S., Adriani, O., Barbarino, G. C., Bazilevskaya, G. A., Bellotti, R., Bogomolov, E. A., Bongi, M., Bonvicini, V., Bruno, A., Cafagna, F., Campana, D., Carlson, P., Casolino, M., Castellini, G., De Santis, C., Galper, A. M., Koldashov, S. V., Koldobskiy, S., Kvashnin, A. N., Leonov, A. A., Malakhov, V. V., Marcelli, L., Martucci, M., Mayorov, A. G., Mergè, M., Mocchiutti, E., Monaco, A., Mori, N., Mikhailov, V. V., Osteria, G., Panico, B., Papini, P., Pearce, M., Picozza, P., Ricci, M., Ricciarini, S. B., Simon, M., Sotgiu, A., Sparvoli, R., Spillantini, P., Stozhkov, Y. I., Vacchi, A., Vannuccini, E., Vasilyev, G. I., Voronov, S. A., Yurkin, Y. T., Zampa, G., Zampa, N.

论文摘要

宇宙辐射中Z = 2分量的精确时间依赖性测量提供了有关带电颗粒通过地球层传播的关键信息。 Pamela实验的长期飞行时间（2006年6月15日至2016年1月23日）和低能阈值（80 MEV/N）是宇宙射线太阳能调制研究的理想检测器。在本文中，介绍了从2006年7月至2009年12月在Carrington旋转时间内通过Pamela仪器测量的氦核光谱。用于宇宙射线传播的最先进的三维模型用于解释时间依赖性的测量通量。还提出了各种刚度的质子与递增的比率时间曲线，以研究可能由不同质量和局部星际光谱形状产生的任何特征。

Precise time-dependent measurements of the Z = 2 component in the cosmic radiation provide crucial information about the propagation of charged particles through the heliosphere. The PAMELA experiment, with its long flight duration (15th June 2006 - 23rd January 2016) and the low energy threshold (80 MeV/n) is an ideal detector for cosmic ray solar modulation studies. In this paper, the helium nuclei spectra measured by the PAMELA instrument from July 2006 to December 2009 over a Carrington rotation time basis are presented. A state-of-the-art three-dimensional model for cosmic-ray propagation inside the heliosphere was used to interpret the time-dependent measured fluxes. Proton-to-helium flux ratio time profiles at various rigidities are also presented in order to study any features which could result from the different masses and local interstellar spectra shapes.

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