Generation and evolution of Solar and Stellar Magnetic Fields, and Implications for the Solar-Stellar Connection
Comparison of 5 models for the evolution of the coronal magnetic field
Date Submitted
2017-04-19 15:41:43
Alan Hood
Erin Goldstraw (St Andrews), Peter Cargill (Imperial), Philippa Browning (Manchester)
University of St Andrews
The slow evolution of the coronal magnetic field is frequently modelled by a sequence to static equiibria. We investigate and compare 5 different methods for studying such an evolution. The coronal magnetic field is slowly stressed by slow photospheric motions. If the loop length is much larger than the loop width then this allows a variety of different approximations to be used. We compare the results using (i) a Magneto-frictional method, (ii) a simple 1D approach, (iii) a linearisation of the MHD equations, (iv) Reduced MHD and finally (v) a full MHD simulation. We investigate when the methods are valid and when they fail.
Schedule
id
Tuesday
date time
09:00 - 10:30
09:52
Abstract
Comparison of 5 models for the evolution of the coronal magnetic field