Frontier physics problems related to the origin of cosmic rays

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Chinese Science Bulletin, Volume 61, Issue 11: 1188-1209(2016) https://doi.org/10.1360/N972015-00702

Frontier physics problems related to the origin of cosmic rays

HongBo HU, YiQing GUO
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  • ReceivedJul 1, 2015
  • AcceptedOct 8, 2015
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Abstract

Ever since the discovery of cosmic rays by Austrian physicist Victor Hess with high altitude balloon experiment in 1912, many fundamental particles as well as their interactions have been discovered in the research of cosmic rays. The first evidence of neutrino oscillation was obtained from the solar neutrino and atmospheric neutrino experiments even though particle physics has been dominated by accelerator experiments. To this day, the highest energy particle is known from the observation of cosmic rays, far beyond the reach of man-made particle accelerator. The origin, acceleration and propagation of cosmic rays are century-old scientific problems. From the studies of cosmic rays, the high energy gamma astronomy, high energy neutrino astronomy and ultra-high energy cosmic rays astronomy have been developed. In order to solve the origin problem, it is helpful to precisely measure the chemical composition and energy spectrum of cosmic rays, to observe and locate the sources of high energy gamma rays, neutrinos and ultra-high energy cosmic rays. Recently, with a new generation of space borne and ground based experiments in operation, great progresses have been made in cosmic ray spectrum and the anisotropy measurement. The fine structure of spectral hardening for primary nuclei at 200 GV was observed by ATIC-2, CREAM and PAMELA. And Positron/electron excesses were discovered by PAMELA and ATIC. The latest results by AMS02 experiment also confirmed the spectral hardening and positron excess with unprecedented precision. In the very high energy range, the knee structure of light elements below PeV has been observed by ARGO-YBJ/LHAASO-WFCTA hybrid experiment with a rather small systematic uncertainty. On the other hand, KASCADE experiment observed a knee at 80 TeV for heavy component and an ankle at 200 PeV for light component. By combining the anisotropy results from Tibet ASg, ARGO-YBJ in northern hemisphere and IceTop in southern hemisphere, a global picture on galactic cosmic ray anisotropy from TeV to PeV energies are now obtained. In the field of high energy neutrino observation, the astrophysical neutrinos with a rather hard spectrum from 30 TeV to 2 PeV have been discovered at a 7.2 significance by IceCube experiment. As for the ultrahigh energy cosmic ray spectrum, AUGER and TA have performed very high precision measurement and their results agree with each other very well. It is worth to note that the composition measurements do not agree with each other when approaching the extremely high energy end. Apparently, GZK cutoff is clearly observed with high significant level. However, alternative explanation, such as the limitation of acceleration power by sources remains possible before the composition is well understood. All these results shed new lights on unveiling the origin of cosmic rays. Besides, these studies are important means to detect the dark matter particle and to explore the evolution of the universe and new laws of physics.


Funded by

国家自然科学基金资助项目(11135010)


Acknowledgment

本文是根据香山会议第518次会议(宇宙线起源的天文和物理交叉研究前沿)的主题评述报告整理而成. 感谢中国科学院高能物理研究所冯朝阳, 博士生田珍和王振在绘图及文献引用方面提供的帮助.


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    图1

    (网络版彩色)太阳系和宇宙线各个元素丰度比较[8]. 其中太阳系各个元素丰度来自于文献[9], 宇宙线丰度来自于文献[10], 质子和氦核丰度来自于文献[11,12]

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    图2

    (网络版彩色)宇宙线能谱: 宇宙线全粒子谱来自于实验观测[16], Tibet-ASg[17], KASCADE[18], Akeno[19], AGASA[20], HiResI[21], HiResII[22], AUGER[23], TA[24], IceCube[25]; 质子成分能谱观测来自于AMS01[26], AMS02[27], BESS[28], ATIC[29], CREAM[30], PAMELA[31], RunJob[32], CAPRICE[33], JACEE[34]; 轻核成分(p+He)观测数据来自于ARGO-YBJ[35], ARGO-WFCTA[36]; 正负电子能谱测量来自于AMS02[37], AMS01[38], PAMELA[39], HEAT[40], CAPRICE[41], ATIC[42], Fermi-LAT[43], HESS[44], BETS[45]; 反质子实验观测来自于PAMELA[46], AMS01[47], BESS[48,49], CAPRICE[50]; 全天区的伽玛射线观测来自于FermiLAT[51]; 大气中微子观测来自于IceCube[52,53], AMANDA[54], ANTARES[55], FREJUS[56]; 天体中微子观测数据来自于文献[57,58]

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    图3

    (网络版彩色)非线性扩散激波加速理论解释宇宙线能谱[79,80]

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    图4

    银河宇宙线至少应该有两个成分[69]

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    图5

    (网络版彩色)p0峰(p0 bump)位于~100 MeV能量[84]

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    图6

    (网络版彩色)(a) 正电子能谱; (b) 负电子能谱. 实验测量数据来自于: AMS02[37], ATIC[42], Fermi-LAT[43], HESS[44], AMS01[38], HEAT[40], CAPRICE[41], BETS[45]

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    图7

    (网络版彩色)(a) 质子能谱; (b) 氦核能谱. 实验测量数据来自于: ATIC[29], CREAM[30], PAMELA[31], AMS02 20152)(footnote: Oliva A, 2013, CERN Courier)

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    图8

    (网络版彩色)(a) 反质子与质子比率; (b) 硼碳比率. 关于pˉ/p的实验观测来自于: PAMELA 2010[116], PAMELA 2014[117], BESS 1995- 1997[118], BESS 1999[119], CAPRICE 1994[120], CAPRICE 1998[121], HEAT[122]. 关于B/C实验观测来自于: AMS02 20133)(footnote: Aguilar M, 2013, CERN Courier), AMS02 20154)(footnote: Oliva A, 2013, CERN Courier), PAMELA[123], RUNJOB[124], Juliusson[125], Dwyer[126], Orth[127], Simon[128], HEAO-3[129], Maehl[130], Voyager[131], Ulysses[132], ACE[133]

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    图9

    (网络版彩色)轻核成分膝区能谱测量结果. 实验观测来自于: ARGO/WFCTA[36,137], ARGO-YBJ[35,138], Tibet-ASg [139], CREAM[30], KASCADE[140]

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    图10

    (网络版彩色)传播模型可以描述“膝”的拐折[141]

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    图11

    大多数的实验测出尖锐的“膝”[142]

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    图12

    (网络版彩色)重核在80 PeV的“膝”及轻核在120 PeV的“踝” [145]

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    图13

    AUGER, TA的精确测量且高度一致的极高能宇宙线能谱[145]

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    图14

    (a) Hillas模型的三分量解释; (b) 极高能增加第四组质子成分[148]

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    图15

    (网络版彩色)TeV能区北天区宇宙线各向异性的二维分布图, 不随时间及太阳活动变化. (a)和(b)中的区域I是所谓的tail-in, 即太阳球磁尾方向, 与太阳所处位置的外旋臂切向接近. 区域II是loss cone方向, 指向接近银河系北极. 区域III是天鹅座方向, 与太阳所处位置的内旋臂切向接近[149]

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    图16

    (网络版彩色)宇宙线各向异性偶极分量的振幅(a)和恒星时相位(b)随能量的变化. 实验观测数据来自于: Norikura1973[153], Ottawa1981[154], London1983[155], Bolivia1985[156], Budapest1985[155], Hobart1985[155], London1985[157], Misato1985[155], Socorro1985[156], Yakutsk1985[155], Baksan1987[158], HongKong1987[159], Sakashita1990[160], Utah1991[161], Liapootah1995[162], Matsushiro1995[163], Poatina1995[164], Kamiokande1997[165], Macro2003[166], SuperKamiokande2007[167], PeakMusal1975[168], Baksan1981[169], Norikura1989[170], Tibet2005[171], EASTOP1995[172], EASTOP1996[173], EASTOP2009[174], Baksan2009[175], Milagro2009[176], ARGO2011[177], IceCube2010[178], IceCube2012[179], IceCube2013[180], Tibet20135)(footnote: Amenomori M, Bi X J, Chen D, et al. Observation of the large-scale sidereal anisotropy of the galactic cosmic ray intensity at 300 TeV with the Tibet Air Shower Array. In: the 33rd International Cosmic Ray Conference. 2013)

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    图17

    (网络版彩色)模拟计算的各向异性振幅随能量变化, 每条线代表一个模拟的银河系情况[181]

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