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作 者:高新亮 马玖琦 邵同 陈瑞 柯阳光 陆全明 Xinliang Gao;Jiuqi Ma;Tong Shao;Rui Chen;Yangguang Ke;Quanming Lu(Deep Space Exploration Laboratory,School of Earth and Space Sciences,University of Science and Technology of China,Hefei 230026,China;CAS Center for Excellence in Comparative Planetology,Hefei 230026,China)
机构地区:[1]Deep Space Exploration Laboratory,School of Earth and Space Sciences,University of Science and Technology of China,Hefei 230026,China [2]CAS Center for Excellence in Comparative Planetology,Hefei 230026,China
出 处:《Science Bulletin》2024年第5期597-600,共4页科学通报(英文版)
基 金:supported by the National Natural Science Foundation of China(42230201 and 42322406);the Strategic Priority Research Program of Chinese Academy of Sciences(XDB41000000);"USTC Tang Scholar"Program。
摘 要:Earth’s diffuse aurora(structureless auroras,5-15 s pulsations and microbursts)occurs over a broad latitude range,which arises from the collision of energetic charged particles with atoms in the upper atmosphere[1].Diffuse aurora exists for most of the time,and intensifies during geo magnetically active periods[2].Although generally not visible to the naked eyes,it is the major source of energy input into the Earth’s nightside upper atmosphere[3].During magnetospheric substorms,~100 eV to 1 keV plasmasheet particles are injected into the midnight sector magnetosphere.Due to the conservation of the particles’first two adiabatic invariants,the particles are energized to~10-100 keV energies.A mechanism that violates the first adiabatic invariant of electrons is required to scatter them to enter the atmospheric loss cone(a small cone of angle~3°wide at the equator)[4].
分 类 号:P427.33[天文地球—大气科学及气象学]
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