ECLAT Cluster Footprint Mapping

ECLAT meeting March 2012 WP330 Cluster footprint mapping 1.Cluster footprint mapping using statistical magnetospheric models for years (10) 2.Time-varying configuration and Cluster footpoint mapping for selected events using adaptive magnetospheric models. 3.Development and testing a new-generation statistical magnetospheric model (T12), adaptation for wide usage 4.Provide input of footprint information to the development of visualization tools (WPs 0440 and 0320); 5.Preparation of final footprint data for ingestion to CAA Main work tasks (m0-m20):

ECLAT meeting March 2012 WP330 Cluster footprint mapping 1.Cluster footprint mapping using statistical magnetospheric models Investigate/select statistical magnetospheric field models most suitable for massive runs ; T96 and TS05 selected Software for mapping, computations of Cluster-3 ionospheric footpoints for (5min time resolution). Provide input of footprint information to the development of visualization tools (WPs 0440 and 0320),

ECLAT meeting March Time-varying configuration and Cluster footprint mapping using adaptive magnetospheric models. Investigate the requirements (spacecraft number /coverage, region,etc) to ensure good quality of adaptive model ( using Themis-time constellations of multi-spacecraft, run the adaptive models for dayside and flank regions (has no value, discarded, see *); Select time intervals with appropriate coverage in the magnetotail ( , Cluster large-scale +GOES + Geotail) Adjust algorithms/codes for using with Cluster and running the adaptive model for identified time intervals; (*) investigation showed: this suggestion was unjustified because, compared to magnetotail case, (1) the number of free model parameters is hard to reduce to a reasonably small number (compared to a number of measurements), and (2) no independent way exists to control the quality of the model constructed (like IsoBoundaries in magnetotail) WP330 Cluster footprint mapping

ECLAT meeting March 2012 WP330 Cluster footprint mapping New-generation empirical magnetospheric model (T12) - new model features : A novel flexible set of separately shielded (at MP) modules describing variable systems of equatorial currents New modules representing global 3d current system (FACs), cusp etc. Model field is confined within a boundary whose size and shape is controlled by the solar wind pressure, geodipole tilt, and IMF Bz. Examples P dyn =6nPa, IMF Bz=+7nT P dyn =6nPa, IMF Bz=-7nT  Variable flaring has a dramatic effect on the global field line configuration, and will have important implications in the modeling of the IMF penetration into the magnetosphere.

ECLAT meeting March 2012 WP330 Cluster footprint mapping New-generation empirical magnetospheric model (T12) - new model features (2): A novel flexible set of separately shielded (at MP) modules describing variable systems of equatorial currents New modules representing global 3d current system (FACs), cusp etc. Model field is confined within a boundary whose size and shape is controlled by the solar wind pressure, geodipole tilt, and IMF Bz. Model is based on vastly extended set of space magnetometer data, largest amount of observations ever used in modeling studies (including new data from Geotail, Polar, Cluster, GOES, Themis … ) Model will be driven by a set of parameters, derived solely from observations in the upstream solar wind, taking into account finite buildup and different relaxation times of magnetospheric current systems, as well as nonlinear saturation effects. That will make it possible to use the model as a short-term forecasting tool.

ECLAT meeting March 2012 WP330 Cluster footprint mapping 3. Develop and test a new-generation statistical magnetospheric model (T12). Develop/test new approaches/modules for different components of 3d current system (last part, R2 -FAC modules to be completed in 04/12) Add new data (collect/compile/verify) to be used for modeling (THEMIS, GOES, Cluster, Polar, etc) ; altogether about 60*satellite*years of new data (records at 5min resolution supplemented by solar wind/IMF tags) Establish optimal combination of IMF/SW parameters, best suited as driving variables for each of the main magnetospheric field source. Assemble the new model, fit the spacecraft database, do initial tests /this model will be comprehensively tested/validated, particularly in application with Cluster, as a part of science /validation efforts at the concluding stage of ECLAT project /