Cosmic Ray Two-Fluid Model¶
New in version 2.2.
For relevant parameters, please also see Cosmic Ray Two-Fluid Model Parameters.
Models dynamical role of cosmic rays via a set of two-fluid hydro equations (see Jun et. al. 1994 ). Central to the effort is a new baryon field, CREnergyDensity, which is in units of ergs/cm^3, and is advected along with the gas. Gradients in the CR field result in a pressure felt by the gas. The CR gas is also diffusive and rays can be produced during star formation. See Cosmic Ray Two-Fluid Model Parameters for information on how to control all these options. But most important:
CRModel- Switches on the CR physics (0 = off, 1 = on)
CRgamma- For polytropic equation of state. 4/3 = relativistic, adiabatic gas (default)
CRDiffusion- turns on diffusion of CREnergyDensity field
CRkappa- Diffusion coefficient (currently constant, isotropic)
CRFeedback- Controls production of rays in star forming regions
For this model to run properly you must be running the Zeus Hydro
HydroMethod = 2. The model has not been implemented for
higher order solvers.
If you plan on including cosmic rays, definitely first verify the solver is working by running the Cosmic Ray Shocktube problem, which ought to match the analytic solution described in Pfrommer 2006 . See the Test Problem Parameter list for more information.
Cosmic Rays have also been implemented in the isolated galaxy simulation. They initialize with
a profile equal to the density of the thermal gas, multiplied by a constant,
set to 0.1 (all in code units).