宇宙线直接探测进展概述
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摘要
宇宙线从发现起至今已超过百年。在20世纪上半叶,大型粒子加速器技术成熟以前,对宇宙线的研究引领着基本粒子物理的发展,从宇宙线研究中取得的多项成果斩获诺贝尔奖。21世纪,宇宙线因其与极端高能的物理规律和暗物质等新物理现象联系密切而绽放出新的活力,宇宙线起源、加速、传播等相关的天文学及物理学问题也备受关注。简述了近年来在空间直接观测宇宙线实验方面取得的进展,以及其对理解宇宙线物理问题的推动。最后概述了中国在相关领域的研究历程和现状。
The history of cosmic ray studies can be traced back to the 1910s when Hess and other scientists first discovered them. Cosmic rays are very important laboratories of particle physics, and led to many important discoveries of fundamental particles such as positrons, muons, pions, and a series of strange particles. Cosmic rays are nowadays key probes of physics at the extremely high energy end and dark matter particles. A brief review about the history and recent progresses of direct observations of cosmic rays is presented. In recent years, new space-borne experiments such as PAMELA and AMS-02, as well as a few balloon-borne experiments, have measured the energy spectra of cosmic rays very precisely and revealed several new features/anomalies. Remarkable excesses of the positron fraction in the total electron plus positron fluxes have been observed, which could be due to dark matter particle annihilation/decay or astrophysical pulsars. The cosmic ray antiprotons, which are expected to have the same secondary origin as that of positrons, do not show significant excesses compared with the background prediction. This result also constrains the modelling of the positron excesses. In addition, spectral hardenings above a few hundred GeV of cosmic ray nuclei have been revealed. Such results have important and interesting implications on our understandings of the origin, acceleration, and propagation of cosmic rays. In particular,China has launched the Dark Matter Particle Explorer(DAMPE) to indirectly search for dark matter and explore the high-energy Universe in the TeV window. Most recently, the DAMPE collaboration reported new measurements of the cosmic ray electron plus positron fluxes up to about 5 TeV with very high precision. The DAMPE data revealed clearly a spectral break around Te V. Possible fine structures of the electron plus positron spectra can be critically addressed with the accumulation of data in the coming years.
The history of cosmic ray studies can be traced back to the 1910s when Hess and other scientists first discovered them. Cosmic rays are very important laboratories of particle physics, and led to many important discoveries of fundamental particles such as positrons, muons, pions, and a series of strange particles. Cosmic rays are nowadays key probes of physics at the extremely high energy end and dark matter particles. A brief review about the history and recent progresses of direct observations of cosmic rays is presented. In recent years, new space-borne experiments such as PAMELA and AMS-02, as well as a few balloon-borne experiments, have measured the energy spectra of cosmic rays very precisely and revealed several new features/anomalies. Remarkable excesses of the positron fraction in the total electron plus positron fluxes have been observed, which could be due to dark matter particle annihilation/decay or astrophysical pulsars. The cosmic ray antiprotons, which are expected to have the same secondary origin as that of positrons, do not show significant excesses compared with the background prediction. This result also constrains the modelling of the positron excesses. In addition, spectral hardenings above a few hundred GeV of cosmic ray nuclei have been revealed. Such results have important and interesting implications on our understandings of the origin, acceleration, and propagation of cosmic rays. In particular,China has launched the Dark Matter Particle Explorer(DAMPE) to indirectly search for dark matter and explore the high-energy Universe in the TeV window. Most recently, the DAMPE collaboration reported new measurements of the cosmic ray electron plus positron fluxes up to about 5 TeV with very high precision. The DAMPE data revealed clearly a spectral break around Te V. Possible fine structures of the electron plus positron spectra can be critically addressed with the accumulation of data in the coming years.
引文
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[68] Strong A W, Moskalenko I V. ApJ, 1998, 509:212
[69] Evoli C, Gaggero D, Grasso D, et al. JCAP, 2008, 10:018
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[71] Aharonian F, Akhperjanian A G, Anton G, et al. A&A, 2009, 508:561
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[73] Yuan Q, Feng L, Yin P F. et al. 2017, arXiv:1711.10989
[74] Zhang S N, Adriani O, Albergo S, et al. SPIE, 2014, 9144:91440X
(1)这类模型假设宇宙线在星际空间中传播时会和随机磁湍流相互作用而获得加速,称为重加速。这类模型可以很好地符合观测到的B/C比例数据~([61])。
(2)假设加速产生的粒子动量谱为单一幂律■,在相对论极限下■,而在非相对论极限下■。
[2] Hess V F. PhZ, 1912, 13:1804
[3] Anderson C D. PhRv, 1933, 43:491
[4] Anderson C D, Neddermeyer S H. PhRv, 1936, 50:263
[5] Rochester G D, Butler C C. Nature, 1947, 160:855
[6] Lattes C M G, Occhialini G P S, Powell C F. Nature, 1947, 160:453
[7] Chang W Y. Rev Mod Phys, 1949, 21:166
[8] Hopper V D, Biswas S. PhRv, 1950, 80:1099
[9] Rossi B B. Ricerca Scienti?ca, 1934, 5:579
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[13] Yoon Y S, Ahn H S, Allison P S, et al. ApJ, 2011, 728:122
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[16] Aguilar M, Ali Cavasonza L, Alpat B, et al. PhRvL, 2017, 119:251101
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[18] Chang J, Adams J H, Ahn H S, et al. Nature, 2008, 456:362
[19] Ambrosi G, An Q, Asfandiyarov R, et al. Nature, 2017, 552:63
[20] Aharonian F, Akhperjanian A G, Barres de Almeida U, et al. PhRvL, 2008, 101:261104
[21] Adriani O, Barbarino G C, Bazilevskaya G A, et al. PhRvL, 2010, 105:121101
[22] Aguilar M, Ali Cavasonza L, Alpat B, et al. PhRvL, 2016, 117:091103
[23] Ackermann M, Ajello M, Albert A, et al. ApJ, 2015, 799:86
[24] Abbasi R U, Abdou Y, Abu-Zayyad T, et al. PhRvD, 2011, 83:012001
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[26] Amenomori M, Bi X J, Chen D, et al. ApJ, 2008, 678:1165
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[30] Yamamoto T. ICRC, 2008, 4:335
[31] Maurin D, Melot F, Taillet R. A&A, 2014, 569:A32
[32] Derbina V A, Galkin V I, Hareyama M, et al. ApJ, 2005, 628:L41
[33] Ahn H S, Allison P, Bagliesi M G, et al. ApJ, 2010, 714:L89
[34] Adriani O, Barbarino G C, Bazilevskaya G A, et al. Nature, 2009, 458:607
[35] Fan Y Z, Zhang B, Chang J. IJMPD, 2010, 19:2011
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[49] Du Vernois M A, Barwick S W, Beatty J J, et al. ApJ, 2001, 559:296
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[65] Strong A W, Moskalenko I V, Ptuskin V S. ARNPS, 2007, 57:285
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[69] Evoli C, Gaggero D, Grasso D, et al. JCAP, 2008, 10:018
[70] Chang J, Ambrosi G, An Q, et al. APh, 2017, 95:6
[71] Aharonian F, Akhperjanian A G, Anton G, et al. A&A, 2009, 508:561
[72] Fang K, Bi X J, Yin P F. ApJ, 2018, 854:57
[73] Yuan Q, Feng L, Yin P F. et al. 2017, arXiv:1711.10989
[74] Zhang S N, Adriani O, Albergo S, et al. SPIE, 2014, 9144:91440X
(1)这类模型假设宇宙线在星际空间中传播时会和随机磁湍流相互作用而获得加速,称为重加速。这类模型可以很好地符合观测到的B/C比例数据~([61])。
(2)假设加速产生的粒子动量谱为单一幂律■,在相对论极限下■,而在非相对论极限下■。