STORMS

To test the shock hypothesis as the prime particle accelerator in the heliosphere, it is essential the further development and the application of novel methods to determine the shock wave dynamics during solar eruptive events. We exploit coronal imagery in different vantage points and wavelengths to locate and map the time varying 3-D expansion of pressure waves and derive their magneto-plasma properties including: the velocity, Mach numbers, compression ratios and geometry in 3-D. Our methods, _that constitute the current state-of-the-art_, reside in forward shock modeling techniques using nearly simultaneous multi-viewpoint white light and EUV observations of pressure/shock waves combined with background coronal and solar wind MHD models to deduce the critical shock parameters in 3-D.

The application of the developed tools and methods during COROSHOCK project allow us to perform:

• Detailed 3-D reconstructions and modeling of coronal shock waves.
• Detailed coupling of the shock wave modelling with magnetic connectivity to evaluate the shock impact on specific regions of the inner heliosphere.
• Detailed analysis of the 3D shock wave properties and connection to SEP and γ-ray events properties.
• [Under-development] The construction of catalog of 3-D reconstructed and modeled shock waves for a plethora of eruptive events.

We account for the physical processes known to operate in the corona and in the interplanetary medium during the acceleration and transport of particles. The production of high-energy particles at the shock will be parameterized using the magneto-plasma shock parameters that are deduced from the 3-D reconstructions and modeling. The result of this parameterization will produce a time varying spectrum of particles at the shock. In addition, we will account for particle transport mechanisms in the interplanetary medium by developing a 3-D particle transport model based on the solution of stochastic differential equations to model the random walk of energetic particles during their propagation to 1AU. This approach is computationally tractable and much simpler to implement numerically than the solution of the full Parker transport equation using finite-difference schemes.

From the application of the acceleration and transport models to the modeled shock waves we will:

• Parameterise the particle energisation and modell particle propagation from the shock to the solar surface to explain the properties of the long-duration >100 MeV γ-ray events.
• Be able to study the longitudinal variability of SEPs through the coupled shock wave and particle transport modeling.
• Exploit the possibility to convert the flux of energetic particles into electromagnetic radiation to produce synthetic γ-ray, hard X-ray, and radio fluxes during highly energetic eruptive events.