MHD inversion of coronal loops
Magnetohydrodynamic (MHD) seismology stands as one of the few indirect methods for the determination of difficult-to- measure physical parameters in solar coronal structures. It relies on the combined use of observed oscillatory properties of MHD waves in solar atmospheric magnetic and plasma structures together with theoretically obtained wave properties.
The code you can download here performs a Bayesian parameter inference in the context of resonantly damped transverse coronal loop oscillations. The forward problem is solved in terms of parametric results for kink waves in one-dimensional flux tubes in the thin tube and thin boundary approximations. The posterior probability distribution functions are obtained by means of an analytical integration of the posterior distribution. An application to several coronal loops can be found in Arregui and Asensio Ramos 2011.
Download
The code can be downloaded from here. Follow the steps in the manual after decompressing the file to compile the code. You will need a Fortran 90 compiler. We have tested it with the Intel Fortran Compiler and with the GNU Fortran Compiler. For any question, contact iarregui@iac.es or aasensio@iac.es