1st year:
1. We have created a complex wave propagation model, consisting of three submodels:
a) magnetospheric propgation
b) transionospheric propgation
c) subionospheric propgation
The submodels have been separately verified. The full model was used to calculate the in-situ VLF power for selected events. The verification of the model is going on.
2. We have developed a code that can read data files from EMMA and ENIGMA magnetometers, perform FFT to obtain power spectral densities for hourly periods, transform those into electric field power spectral densities at the equator in space, and derive hourly values of the electric field radial diffusion coefficient. We have also added a functionality for including an assessed contribution of the magnetic field radial diffusion coefficient, using a statistical approximation that links the two, however imperfectly; and performed initial tests on historical dates of quiet and active geomagnetic conditions.
3. We have developed a method for the definition, automatic detection and analysis of the events In the Radiation Belts using Ca index.
4. We have implemented the Analog Ensemble method to provide scenario-based forecasts for FARBES.
2nd-3rd year:
1. We have validated the wave propagation model through simultaneous measurements from ground VLF data and Van Allen Probes burst mode data. We have developed a neural-network based (YOLO v11) chorus detector and used it to identify chorus event in ground and in-situ data. From the identified chorus events, the wave powers were extracted and then, using the wave propagation model developed in the 1st year, the estimated wave powers were calculated. These wave powers were used as proxies to scale the Salammbo VLF wave power statistics.
2.We have extended the method to derive the electric term of t the radial diffusion coefficient based on on ground ULF measurements. The method was validated by using in-situ data measured by the THEMIS spacecrafts. The diffusion coefficients were then integrated to Salammbô code.
3. We have developed a dynamic VLF wave power statistics based on solar wind event classes (CIR, CME and CIR+CME), magnetic activity (four AE index classes) and in-situ wave data from several satellite instruments, such as THEMIS A (FFT), CLUSTER 1 (STAFF SA), DE1 (PWI), POLAR (PWI), RBSP A (EMFISIS), creating a binned (L*/MLT/Activity/AE) chorus wave power statistics.
4. Salammbo simulations using Analog Ensemble method were run on two event scenarios (Ca75 (03/2015) and Ca90 (08/2015) events) using diffusion coefficients obtained from ground based VLF and ULF measurements. The simulation results are superior to the one based on diffusion coefficients obtained form Salammbo default wave power statistics and on certain energy ranges are better than the one based on the new dynamic wave power statistics.