P-CORONA

P-CORONA is a novel computer program for modeling the intensity and polarization of coronal atomic lines in any given three dimensional (3D) model of the solar corona. It takes into account the scattering of anisotropic radiation as well as the symmetry-breaking effects arising from the influence of magnetic fields, through the Hanle and Zeeman effects, and from non-radial solar wind velocities. To this end, P-CORONA solves the statistical equilibrium equations for the elements of the atomic density matrix corresponding to the multi-level atomic model under consideration, assuming complete frequency redistribution (see chapter 7 of Landi Degl'Innocenti & Landolfi 2004). The calculations are carried out assuming an optically thin plasma, with the emergent Stokes profiles resulting from the integration of the local emission coefficients along the line-of-sight in the chosen 3D coronal model. P-CORONA incorporates HDF5 input/output functionality and includes a graphical user interface. The code has been developed, and is made publicly available, within the framework of the POLMAG project.

References

The main reference for the code that you should give when publishing papers using P-CORONA is:

• Supriya H.D., Trujillo Bueno J., de Vicente A., del Pino Alemán T. 2021, Polarization of the Lyα Lines of H I and He II as a Tool for Exploring the Solar Corona ApJ, 920(2):140

Download

The code is freely available to the community, hosted at GitLab. The latest version of P-CORONA can be found at https://gitlab.com/polmag/P-CORONA, and the latest version of the documentation at https://polmag.gitlab.io/P-CORONA/.