Surface Flux Transport 1D documentation

We can only observe half of the solar surface routinely. However, a global observation is essential for understanding and forecasting solar activity. Sun is magnetically active and this activity cycle lasts for about 11 years during which the magnetic field distribution on the solar surface – the photosphere, evolves and generates a vast range of events e.g., emergece and decay of sunspots, solar flares, coronal mass ejections, flow of solar wind and energetic particles into the heliosphere etc. In order to understand these we can use theoretical models to compute the global magnetic field configuration on the photosphere and later use them to drive different models. Surface flux transport model solves the radial component of the magnetic induction equation on the solar surface by using prescribed flow profiles and source terms. This distribution provides a numerical model of SFT developed in FORTRAN by folowing Yeates (2020).

Link to the GitHub repository: https://sr-dash.github.io/SFT-1D/.

Link to the resources used in Yeates (2020): sharps-bmrs.

Here is a short guide on how to build the SFT 1D code, install the dependencies and check the output.

Contents:

• Quick Start
  • Acknowledgments
  • System Requirements
  • A Brief Description of the SFT 1D code
  • General Hints
• Sample plotting routine for SFT 1D
• Theoretical background
  • Magnetic field evolution on the solar surface
  • BMR modeling algorithm