Speaker
Nicholas Owens
(McMaster University)
Description
Today, large scale galaxy simulations take advantage of magneto-hydrodynamics, relying on a continuum approximation of interstellar gas. This, in turn, relies on the assumption that the mean free path is well below the resolution of the simulation. This is true for many ISM processes but becomes less reliable when introducing the hot plasma found in superbubbles or the CGM.
Our work outlines the need for additional physics, depending on the nature of the simulations being used. In low order corrections, this takes the form of diffusive and resistive processes. We also introduce hyperbolic conduction, a more physical form of conduction, to take the mean free path into account in our simulations.
Primary author
Nicholas Owens
(McMaster University)
Co-author
Dr
James Wadsley
(McMaster University)
