Wavelet-based modeling of the heliospheric turbulent magnetic field

We present a model of the magnetic field in the heliosphere. Our model's magnetic field is made of a large-scale component, modeled as the Parker Spiral, and a small-scale turbulence component, modeled through a wavelet-based method. The turbulent component is tailored to reproduce a few key properties of magnetic fluctuations in the Parker Spiral, such as a varying correlation length and a decreasing turbulence amplitude as a function of the radial distance from the Sun. The wavelet-based method is obtained from a previously developed Cartesian method by defining a new set of coordinates to ensure the correct scaling of the turbulence correlation length as a function of the radial distance. Our algorithm allows for reproducing a larger spectral range of fluctuations than magnetohydrodynamic simulations, which is needed to properly describe the gyroresonant scattering of energetic particles. In the future, the model will be used to study energetic particle propagation in the heliosphere.