Modelling the heliospheric magnetic field through wavelet-based synthetic turbulence

We present a model of the heliospheric magnetic field that combines a large-scale Parker Spiral component with a small-scale turbulent contribution generated using a wavelet-based approach. The turbulent fluctuations are constructed to reproduce key properties of magnetic turbulence observed in the expanding solar wind, including a radially decreasing amplitude and a spatially varying correlation length. The wavelet-based method is adapted from a previously developed Cartesian model through the introduction of a new coordinate system, which ensures the correct radial scaling of the turbulence correlation length. This approach allows us to model a wider spectral range of fluctuations than is typically achievable with magnetohydrodynamic simulations, a crucial requirement for accurately describing gyroresonant scattering of energetic particles. The model is designed for future applications in studies of energetic particle transport in the heliosphere.