The EISCAT data are used to confirm the important role of precipitation particles in the ionization rate in the auroral region. The height range of the effective ionization is quite different for particles with differ...The EISCAT data are used to confirm the important role of precipitation particles in the ionization rate in the auroral region. The height range of the effective ionization is quite different for particles with different energies. On the other hand, an enhancement of magnetospheric convection often results in decreasing of electron density, N , in the F layer. During January 28 ̄29,1985, the disturbed profiles of N were very typical, in which N m(E layer) N (F layer) and N decreased with height above 147 km. This phenomenan is caused by both energetic particles and intensive convection. During the period of February 16 ̄17, 1993, however, the N (F layer) increased extremely, while N (E layer) remained low. This is also a typical profile, but is opposite to the former one. In this case,the particles with lower energy (<1 keV) in the magnetosheath enter directly the high latitude ionosphere through the cusp,and can contribute significantly to the F layer ionization content.展开更多
太阳风向磁层-电离层(Magnetosphere and Ionosphere,MI)系统输入能量,而输入的能量随后在MI系统中消耗.本文从能量守恒原理出发,讨论太阳风-磁层-电离层(SMI)耦合过程中的能流路径和能量收支的定量关系.主要讨论9个问题:(1)太阳风向MI...太阳风向磁层-电离层(Magnetosphere and Ionosphere,MI)系统输入能量,而输入的能量随后在MI系统中消耗.本文从能量守恒原理出发,讨论太阳风-磁层-电离层(SMI)耦合过程中的能流路径和能量收支的定量关系.主要讨论9个问题:(1)太阳风向MI系统的能量输入,(2)MI系统对能量输入的响应,(3)环电流的能量消耗,(4)极区电离层焦耳加热的能量消耗,(5)极光粒子沉降的能量消耗,(6)磁尾能量的消耗、储存以及返回下游太阳风,(7)平静期间的能量积累与释放,(8)能量在不同能汇中的分配,(9)评价能量函数的准则和方法.展开更多
文摘The EISCAT data are used to confirm the important role of precipitation particles in the ionization rate in the auroral region. The height range of the effective ionization is quite different for particles with different energies. On the other hand, an enhancement of magnetospheric convection often results in decreasing of electron density, N , in the F layer. During January 28 ̄29,1985, the disturbed profiles of N were very typical, in which N m(E layer) N (F layer) and N decreased with height above 147 km. This phenomenan is caused by both energetic particles and intensive convection. During the period of February 16 ̄17, 1993, however, the N (F layer) increased extremely, while N (E layer) remained low. This is also a typical profile, but is opposite to the former one. In this case,the particles with lower energy (<1 keV) in the magnetosheath enter directly the high latitude ionosphere through the cusp,and can contribute significantly to the F layer ionization content.
文摘太阳风向磁层-电离层(Magnetosphere and Ionosphere,MI)系统输入能量,而输入的能量随后在MI系统中消耗.本文从能量守恒原理出发,讨论太阳风-磁层-电离层(SMI)耦合过程中的能流路径和能量收支的定量关系.主要讨论9个问题:(1)太阳风向MI系统的能量输入,(2)MI系统对能量输入的响应,(3)环电流的能量消耗,(4)极区电离层焦耳加热的能量消耗,(5)极光粒子沉降的能量消耗,(6)磁尾能量的消耗、储存以及返回下游太阳风,(7)平静期间的能量积累与释放,(8)能量在不同能汇中的分配,(9)评价能量函数的准则和方法.