Data acquired by imaging relative ionospheric opacity meters(riometers),ionospheric total electron content(TEC)monitors,and three-wavelength auroral imagers at the conjugate Zhongshan station(ZHS)in Antarctica and Yel...Data acquired by imaging relative ionospheric opacity meters(riometers),ionospheric total electron content(TEC)monitors,and three-wavelength auroral imagers at the conjugate Zhongshan station(ZHS)in Antarctica and Yellow River station(YRS)in the Arctic were analyzed to investigate the response of the polar ionosphere to an interplanetary shock event induced by solar flare activity on July 12,2012.After the arrival of the interplanetary shock wave at the magnetosphere at approximately 18:10 UT,significantly enhanced auroral activity was observed by the auroral imagers at the ZHS.Additionally,the polar conjugate observation stations in both hemispheres recorded notable evolution in the two-dimensional movement of cosmic noise absorption.Comparison of the ionospheric TEC data acquired by the conjugate pair showed that the TEC at both sites increased considerably after the interplanetaryshock wave arrived,although the two stations featured different sunlight conditions(polar night in July in the Antarctic region and polar day in the Arctic region).However,the high-frequency(HF)coherent radar data demonstrated that different sourcesmight be responsible for the electron density enhancement in the ionosphere.During the Arctic polar day period in July,the increased electron density over YRS might have been caused by anti-sunward convection of the plasma irregularity,whereas in Antarctica during the polar night,the increased electron density over ZHS might have been caused by energetic particle precipitation from the magnetotail.These different physical processes might be responsible for the different responses of the ionosphere at the two conjugate stations in response to the same interplanetary shock event.展开更多
Substorm processes have been studied in detail,and it is well known that interplanetary(IP)shock encountering the terrestrial magnetosphere causes global responses.However,how IP shock compression to the magnetosphere...Substorm processes have been studied in detail,and it is well known that interplanetary(IP)shock encountering the terrestrial magnetosphere causes global responses.However,how IP shock compression to the magnetosphere affects the development of an ongoing substorm remains uninvestigated.Herein,the simultaneous satellite and ground-based auroral evolutions associated with an IP shock impact on the magnetopause during an ongoing substorm on May 7th,2005,were examined.The IMAGE satellite over the Southern Hemisphere captured the global development substorm,which was initiated at 17:38:47 UT.The poleward branch of the nightside auroral oval was fortuitously monitored by an all-sky camera at the Zhongshan Station(-74.5°magnetic latitude,ZHO)in Antarctica.The satellite imager observed continuous brightening and broadening of the nightside auroral oval after the IP shock arrival.The simultaneous ground-based optical aurora measurement displayed the intensification and expansion of a preexisting auroral surge poleward of the aurora oval.The geomagnetic field variations and the instantly increased PC indices indicated an elevated merging rate and enhanced the convection-related DP-2 currents.Therefore,this IP shock transient impact did not significantly change the ongoing development of the substorm,although it meets the magnetospheric precondition hypothesis.展开更多
Two THEMIS(Time History of Events and Macroscale Interactions during Substorms)spacecraft,B and C,began orbiting the Moon in 2011 and have since provided routine measurements of the plasma conditions in the lunar orbi...Two THEMIS(Time History of Events and Macroscale Interactions during Substorms)spacecraft,B and C,began orbiting the Moon in 2011 and have since provided routine measurements of the plasma conditions in the lunar orbit.In this study,we systematically compare these measurements in near-Earth space with solar wind measurements obtained from the Lagrangian 1(L1)point and propagated to the Earth,including measurements in the OMNI database and from the Wind spacecraft.A statistical comparison between THEMIS data and data from the OMNI database from September 2011 to December 2017 showed that the Y and Z components of the magnetic field and the flow speed are generally consistent between the two data sets.The ion number density and the dynamic pressure measured by THEMIS in near-Earth space are lower than those in the OMNI database,suggesting possible variation in the solar wind environment while propagating from the L1 point to near-Earth space.We further show two examples in which near-Earth solar wind measurements are applied in calculating the magnetopause location and in quantifying the magnetic field response to interplanetary shocks.Both examples suggest that using solar wind data from near-Earth space achieves better results than using solar wind data from the L1 point.These results provide validation of THEMIS-B and THEMIS-C as an alternative monitor of the near-Earth solar wind environment.展开更多
Based on cosmic ray data obtained by neutron monitors at the Earth＇s surface, and data on near-relativistic electrons measured by the WIND satellite, as well as on solar X-ray and radio burst data, the solar energeti...Based on cosmic ray data obtained by neutron monitors at the Earth＇s surface, and data on near-relativistic electrons measured by the WIND satellite, as well as on solar X-ray and radio burst data, the solar energetic particle （SEP） event of 2005 January 20 is studied. The results show that this event is a mixed event where the flare is dominant in the acceleration of the SEPs, the interplanetary shock accelerates mainly solar protons with energies below 130 MeV, while the relativistic protons are only accelerated by the solar flare. The interplanetary shock had an obvious acceleration effect on relativistic electrons with energies greater than 2 MeV. It was found that the solar release time for the relativistic protons was about 06：41 UT, while that for the near-relativistic electrons was about 06：39 UT. The latter turned Out to be about 2 rain later than the onset time of the interplanetary type HI burst.展开更多
This paper studies the effects of the solar wind on Jupiter’s magnetosphere. The solar wind parameters are characterized using the Michigan Solar Wind Model (mSWiM) solar wind data propagated to Jupiter from 1997 to ...This paper studies the effects of the solar wind on Jupiter’s magnetosphere. The solar wind parameters are characterized using the Michigan Solar Wind Model (mSWiM) solar wind data propagated to Jupiter from 1997 to 2016. This analysis covers almost solar cycles 23 and 24. Interplanetary fast shocks: Forward shocks (FS), Reverse shocks (RS), and solar wind dynamic pressure were obtained and analyzed during the apparent opposition periods. The fast forward (FS) shocks were predominant during this period. Generally, the solar wind dynamic pressure from FS and RS shocks follows the solar cycles 23 and 24.展开更多
We investigate the magnetospheric response to the 17 March 2015 interplanetary(IP)shock using coordinated groundbased global navigation satellite system(GNSS)total electron content(TEC)observations and global magnetoh...We investigate the magnetospheric response to the 17 March 2015 interplanetary(IP)shock using coordinated groundbased global navigation satellite system(GNSS)total electron content(TEC)observations and global magnetohydrodynamic(MHD)simulations.The TEC measurements reveal distinct perturbations induced by the shock,with the MHD model successfully reproducing the qualitative features of these variations.Our analysis demonstrates:(1)TEC signatures of fast-mode MHD wave propagation from the magnetopause to the inner magnetosphere/plasmasphere within 70 s,generating the strongest TEC enhancements near the subsolar point;(2)subsequent wave reflection between the plasmasphere and magnetopause,producing a secondary TEC peak approximately 2 min after the initial impulse.Comparisons with ground magnetometer data show synchronized two-peak structures,supporting the interpretation of wave reflection dynamics.Although the MHD simulations systematically underestimate TEC magnitudes due to the exclusion of cold plasmaspheric populations,they validate the global patterns and timing of the shock response revealed by the TEC observations.These findings highlight the unique capability of GNSS TEC measurements,with their global coverage and high temporal resolution,to complement in situ observations for studying global-scale magnetospheric wave dynamics and shock impacts.The study underscores the potential of GNSS networks as a powerful tool for probing magnetospheric plasma dynamics,particularly in regions lacking direct satellite instrumentation.展开更多
基金the National Key R&D Program of China(Grant no.2018YFF01013706)the National Natural Science Foundation of China(Grant no.41831072)the Top-Notch Young Talents Program of China(Grant no.W02070249).
文摘Data acquired by imaging relative ionospheric opacity meters(riometers),ionospheric total electron content(TEC)monitors,and three-wavelength auroral imagers at the conjugate Zhongshan station(ZHS)in Antarctica and Yellow River station(YRS)in the Arctic were analyzed to investigate the response of the polar ionosphere to an interplanetary shock event induced by solar flare activity on July 12,2012.After the arrival of the interplanetary shock wave at the magnetosphere at approximately 18:10 UT,significantly enhanced auroral activity was observed by the auroral imagers at the ZHS.Additionally,the polar conjugate observation stations in both hemispheres recorded notable evolution in the two-dimensional movement of cosmic noise absorption.Comparison of the ionospheric TEC data acquired by the conjugate pair showed that the TEC at both sites increased considerably after the interplanetaryshock wave arrived,although the two stations featured different sunlight conditions(polar night in July in the Antarctic region and polar day in the Arctic region).However,the high-frequency(HF)coherent radar data demonstrated that different sourcesmight be responsible for the electron density enhancement in the ionosphere.During the Arctic polar day period in July,the increased electron density over YRS might have been caused by anti-sunward convection of the plasma irregularity,whereas in Antarctica during the polar night,the increased electron density over ZHS might have been caused by energetic particle precipitation from the magnetotail.These different physical processes might be responsible for the different responses of the ionosphere at the two conjugate stations in response to the same interplanetary shock event.
基金supported by the National Key R&D Program of China(Grant No.2021YFE0106400)the National Scientific Foundation of China(Grant Nos.42120104003,41974185 and 42130210)+3 种基金Shanghai Science and Technology Innovation Action Plan(Grant Nos.21DZ1206100 and 22ZR1481200)SOA Key Laboratory for Polar Science(Grant No.KP201703)Chinese Meridian ProjectMNR Innovative Youth Talents Program(Grant No.12110600000018003921)。
文摘Substorm processes have been studied in detail,and it is well known that interplanetary(IP)shock encountering the terrestrial magnetosphere causes global responses.However,how IP shock compression to the magnetosphere affects the development of an ongoing substorm remains uninvestigated.Herein,the simultaneous satellite and ground-based auroral evolutions associated with an IP shock impact on the magnetopause during an ongoing substorm on May 7th,2005,were examined.The IMAGE satellite over the Southern Hemisphere captured the global development substorm,which was initiated at 17:38:47 UT.The poleward branch of the nightside auroral oval was fortuitously monitored by an all-sky camera at the Zhongshan Station(-74.5°magnetic latitude,ZHO)in Antarctica.The satellite imager observed continuous brightening and broadening of the nightside auroral oval after the IP shock arrival.The simultaneous ground-based optical aurora measurement displayed the intensification and expansion of a preexisting auroral surge poleward of the aurora oval.The geomagnetic field variations and the instantly increased PC indices indicated an elevated merging rate and enhanced the convection-related DP-2 currents.Therefore,this IP shock transient impact did not significantly change the ongoing development of the substorm,although it meets the magnetospheric precondition hypothesis.
基金supported by the National Natural Science Foundation of China (grants 41821003 and 41974194)
文摘Two THEMIS(Time History of Events and Macroscale Interactions during Substorms)spacecraft,B and C,began orbiting the Moon in 2011 and have since provided routine measurements of the plasma conditions in the lunar orbit.In this study,we systematically compare these measurements in near-Earth space with solar wind measurements obtained from the Lagrangian 1(L1)point and propagated to the Earth,including measurements in the OMNI database and from the Wind spacecraft.A statistical comparison between THEMIS data and data from the OMNI database from September 2011 to December 2017 showed that the Y and Z components of the magnetic field and the flow speed are generally consistent between the two data sets.The ion number density and the dynamic pressure measured by THEMIS in near-Earth space are lower than those in the OMNI database,suggesting possible variation in the solar wind environment while propagating from the L1 point to near-Earth space.We further show two examples in which near-Earth solar wind measurements are applied in calculating the magnetopause location and in quantifying the magnetic field response to interplanetary shocks.Both examples suggest that using solar wind data from near-Earth space achieves better results than using solar wind data from the L1 point.These results provide validation of THEMIS-B and THEMIS-C as an alternative monitor of the near-Earth solar wind environment.
基金Supported by the National Natural Science Foundation of China.
文摘Based on cosmic ray data obtained by neutron monitors at the Earth＇s surface, and data on near-relativistic electrons measured by the WIND satellite, as well as on solar X-ray and radio burst data, the solar energetic particle （SEP） event of 2005 January 20 is studied. The results show that this event is a mixed event where the flare is dominant in the acceleration of the SEPs, the interplanetary shock accelerates mainly solar protons with energies below 130 MeV, while the relativistic protons are only accelerated by the solar flare. The interplanetary shock had an obvious acceleration effect on relativistic electrons with energies greater than 2 MeV. It was found that the solar release time for the relativistic protons was about 06：41 UT, while that for the near-relativistic electrons was about 06：39 UT. The latter turned Out to be about 2 rain later than the onset time of the interplanetary type HI burst.
文摘This paper studies the effects of the solar wind on Jupiter’s magnetosphere. The solar wind parameters are characterized using the Michigan Solar Wind Model (mSWiM) solar wind data propagated to Jupiter from 1997 to 2016. This analysis covers almost solar cycles 23 and 24. Interplanetary fast shocks: Forward shocks (FS), Reverse shocks (RS), and solar wind dynamic pressure were obtained and analyzed during the apparent opposition periods. The fast forward (FS) shocks were predominant during this period. Generally, the solar wind dynamic pressure from FS and RS shocks follows the solar cycles 23 and 24.
基金supported by the Key Innovation Team of China Meteorological Administration“Space Weather Monitoring and Alerting”(Grant No.CMA2024ZD01)the“Ionospheric Forecast and Alerting”Youth Innovation Team(Grant No.CMA2024QN09)the Chinese Meridian Project,and the National Natural Science Foundation of China(Grant No.42374186)。
文摘We investigate the magnetospheric response to the 17 March 2015 interplanetary(IP)shock using coordinated groundbased global navigation satellite system(GNSS)total electron content(TEC)observations and global magnetohydrodynamic(MHD)simulations.The TEC measurements reveal distinct perturbations induced by the shock,with the MHD model successfully reproducing the qualitative features of these variations.Our analysis demonstrates:(1)TEC signatures of fast-mode MHD wave propagation from the magnetopause to the inner magnetosphere/plasmasphere within 70 s,generating the strongest TEC enhancements near the subsolar point;(2)subsequent wave reflection between the plasmasphere and magnetopause,producing a secondary TEC peak approximately 2 min after the initial impulse.Comparisons with ground magnetometer data show synchronized two-peak structures,supporting the interpretation of wave reflection dynamics.Although the MHD simulations systematically underestimate TEC magnitudes due to the exclusion of cold plasmaspheric populations,they validate the global patterns and timing of the shock response revealed by the TEC observations.These findings highlight the unique capability of GNSS TEC measurements,with their global coverage and high temporal resolution,to complement in situ observations for studying global-scale magnetospheric wave dynamics and shock impacts.The study underscores the potential of GNSS networks as a powerful tool for probing magnetospheric plasma dynamics,particularly in regions lacking direct satellite instrumentation.
