THe effects of strong convection electric field on the electron density in the auroral ionosphericF-region have been simulated numerically by means of a physical model. It is found that an enhancement of electric fiel...THe effects of strong convection electric field on the electron density in the auroral ionosphericF-region have been simulated numerically by means of a physical model. It is found that an enhancement of electric field directed west-northward in post-noon or west-southward in pre-noon results in an ionization depletion with its maximum at altitudes 40–50 km higher than that of theF 2 peak. When the enhanced electric field lasts for 45 min and has a maximum about 32 mV/m, the resulted ionization depletions reach their maximum at the time just ～10 min behind the time when the convection electric field and ion temperature enhancements reach their maximum. This is consistent well with EISCAT observations. The magnitudes of the percentage ionization depletions and their recovery time are dependent not only on the intensity of the electric field, but also on the diurnal variation phase of the background electron density.展开更多
The Graz Ionospheric Flux Tube Simulations （GIFTS） has been improved. The improved GIFTS model was used to numerically investigate the energy particle precipitation on the distribution of electron density in the ion...The Graz Ionospheric Flux Tube Simulations （GIFTS） has been improved. The improved GIFTS model was used to numerically investigate the energy particle precipitation on the distribution of electron density in the ionospheric cusp foot-point region under conditions of large plasma convection during magnetic storm. After including the effects of low energy incident particles, the ionospheric electron densities increase remarkably above altitude of -250 km, showing a peak at about 350 km. The percent enhancements of electron densities increase gradually with altitude, exceed- ing 60% near the upper boundary of the calculation. The calculated ionospheric F2-peak was remarkably enhanced and lifted up by the incident low energy electrons.展开更多
We have examined the Wind data in 1996 and identified 21 small interplanetary magnetic flux ropes(SIMFRs),and all the 21 SIMFRs have boundary layer structures.The durations of the boundary layers varied from several m...We have examined the Wind data in 1996 and identified 21 small interplanetary magnetic flux ropes(SIMFRs),and all the 21 SIMFRs have boundary layer structures.The durations of the boundary layers varied from several minutes to 30 minutes.These boundary layers also have properties of high proton temperature,density,and plasma beta.These boundary layers are formed by magnetic reconnections.In addition,in three events magnetic reconnections were occurring inside the boundary layers.It indicates that the flux rope structures have propagated for some period of time,and their boundaries were still evolving through interaction with the background solar wind.Namely it is very possible that the SIMFRs came from the solar corona.展开更多
Since their use in the study of charged particle motion in the 1960s,Euler potentials(α ,β)have been widely employed as magnetic field coordinates in both space plasma and fusion plasma studies.People related them t...Since their use in the study of charged particle motion in the 1960s,Euler potentials(α ,β)have been widely employed as magnetic field coordinates in both space plasma and fusion plasma studies.People related them to magnetic vector potential A via the relation A=α▽β subject to gauge condition A·B=0(B is the magnetic induction).For a given magnetic field,the Euler potentials are often constructed with the relation B·△ S=△α△βon a surface that crosses the field lines,where △ S is the area-element surrounding by two line-elements corresponding to the changes in α and β,then mapping the values of α and βalong field lines into space.In this short paper,we show that in the presence of field line-aligned currents,the mapping does not work and the orthogonality gauge condition is not satisfied.展开更多
基金the National Natural Science Foundation of China (496742 4140 0 740 3 9) and the Research Fund forthe Doctoral Program of Higher Education in China
文摘THe effects of strong convection electric field on the electron density in the auroral ionosphericF-region have been simulated numerically by means of a physical model. It is found that an enhancement of electric field directed west-northward in post-noon or west-southward in pre-noon results in an ionization depletion with its maximum at altitudes 40–50 km higher than that of theF 2 peak. When the enhanced electric field lasts for 45 min and has a maximum about 32 mV/m, the resulted ionization depletions reach their maximum at the time just ～10 min behind the time when the convection electric field and ion temperature enhancements reach their maximum. This is consistent well with EISCAT observations. The magnitudes of the percentage ionization depletions and their recovery time are dependent not only on the intensity of the electric field, but also on the diurnal variation phase of the background electron density.
基金the National Natural Science Foundation o China(40404015, 40390150)the Open Foundation of the Key Laboratory o Geospace Environment and Geodesy of Ministry of Education
文摘The Graz Ionospheric Flux Tube Simulations （GIFTS） has been improved. The improved GIFTS model was used to numerically investigate the energy particle precipitation on the distribution of electron density in the ionospheric cusp foot-point region under conditions of large plasma convection during magnetic storm. After including the effects of low energy incident particles, the ionospheric electron densities increase remarkably above altitude of -250 km, showing a peak at about 350 km. The percent enhancements of electron densities increase gradually with altitude, exceed- ing 60% near the upper boundary of the calculation. The calculated ionospheric F2-peak was remarkably enhanced and lifted up by the incident low energy electrons.
基金supported by the National Natural Science Foundation of China(41074124,40804034 and 40890162)the Program for Science & Technology Innovation Talents in Universities of Henan Province(HASTIT)(2010HASTIT022)the Specialized Research Fund for State Key Laboratories and Key Laboratory of Solar Activity and the Program for Science & Technology of Henan(092300410189)
文摘We have examined the Wind data in 1996 and identified 21 small interplanetary magnetic flux ropes(SIMFRs),and all the 21 SIMFRs have boundary layer structures.The durations of the boundary layers varied from several minutes to 30 minutes.These boundary layers also have properties of high proton temperature,density,and plasma beta.These boundary layers are formed by magnetic reconnections.In addition,in three events magnetic reconnections were occurring inside the boundary layers.It indicates that the flux rope structures have propagated for some period of time,and their boundaries were still evolving through interaction with the background solar wind.Namely it is very possible that the SIMFRs came from the solar corona.
基金supported by the National Natural Science Foundation of China(10973043 and 41074107)the National Basic Research Program of China(2011CB811402)
文摘Since their use in the study of charged particle motion in the 1960s,Euler potentials(α ,β)have been widely employed as magnetic field coordinates in both space plasma and fusion plasma studies.People related them to magnetic vector potential A via the relation A=α▽β subject to gauge condition A·B=0(B is the magnetic induction).For a given magnetic field,the Euler potentials are often constructed with the relation B·△ S=△α△βon a surface that crosses the field lines,where △ S is the area-element surrounding by two line-elements corresponding to the changes in α and β,then mapping the values of α and βalong field lines into space.In this short paper,we show that in the presence of field line-aligned currents,the mapping does not work and the orthogonality gauge condition is not satisfied.
