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The January 10, 1997 interplanetary high-speed stream and the resultant first substorm is studied using Wind interplanetary data and Polar UV images, respectively.
We use WIND solar wind data a POLAR UV imaging data to study magnetospheric responses and substorm triggering mechanisms during and after interplanetary (IP) shock events.
We use WIND solar wind data and POLAR UV imaging data to study magnetospheric responses and substorm triggering mechanisms during and after interplanetary (IP) shock events.
We use WIND solar data and POLAR UV imaging data to study magnetospheric responses and substorm triggering mechanisms during and after interplanetary (IP) shock events.
We use 1997-1998 Wind Solar Wind data and POLAR UV imaging data to study magnetospheric responses and substorm triggering mechanisms during and after interplanetary (IP) shock events.
Ten interplanetary WIND shock/ pressure pulse events are used to study the magnetospheric delay of pseudobreakup (PB) or substorm onsets. We identify the PBs and substorms by using the POLAR UV imaging data. The states of the interplanetary medium and the conditions of the ionosphere before and after the auroral brightening onsets are studied. We find that the magnetospheric delay time strongly constrains the location of the nightside X-line during such events. We also find for PB (or no activity) events, that the interplanetary and ionosphere preconditions are unusually low.
We statistically analyze many interplanetary shock events where there are both WIND interplanetary data and POLAR UV imaging data. We find that the shock compression events trigger pseudobreakups (PBs), substorm onsets, or enhance (pre-existing) substorm intensities. Using WIND interplanetary data and ground-based data, it is now believed that we can predict when PBs will occur and when substorm expansion phases will occur.
Responses of the nightside magnetosphere and auroral zone to interplanetary shocks are studies using WIND solar wind data and POLAR UV imaging data.