Description
One of the fundamental structures found within the solar corona are loops of dense plasma and high magnetic flux. Under the extreme conditions found within the solar atmosphere, thermal transport can both become limited and non-local. An MHD code, with a non-local thermal conduction model included is used to investigate its effect on the solar atmosphere. In particular it is used to simulate a stable coronal loop and investigate how the properties of the loop, including its apex temperature and length, scale with each other. It is found that the non-local conduction model produces a higher apex temperature $T$ and lower apex density than those obtained using purely local conduction. However the dependence of these properties on the loop length $L$ and coronal heating term $H$ remain largely unchanged between the different models. These results are contextualised in reference to the loop scaling laws as derived by Rosner, Tucker and Vaiana.
