Changes between Version 3 and Version 4 of AstroBearProjects/AblativeRT


Ignore:
Timestamp:
01/07/14 21:40:54 (11 years ago)
Author:
Shule Li
Comment:

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  • AstroBearProjects/AblativeRT

    v3 v4  
    1717The boundary condition of this problem is: periodic on x direction, and hydrostatic at y up. The y bottom boundary condition is much trickier because we need to fix the heat flux. This condition involves first solve the boundary temperature using the nonlinear diffusion equation, then using this temperature to find out the density that satisfies the quasi-hydrostatic requirement. Following is a more detailed discussion on the RT boundary condition.[[BR]]
    1818[http://www.pas.rochester.edu/~shuleli/0706/boundary.pdf open pdf]
     19
     20== Diffusive RT ==
     21The difference between the diffusive RT and the ablative RT is that in this case, we do not have a heat flux at the bottom of the simulation box. The results can be seen on this webpage:[[BR]]
     22http://www.pas.rochester.edu/~shuleli/frame_0328.htm
     23[[BR]][[BR]]
     24
     25== Magneto Thermal Instability ==
     26To test the magnetized thermal conduction, we investigate the MTI growth rate. The results are summarized on the following webpage:[[BR]]
     27http://www.pas.rochester.edu/~shuleli/frame_1020.htm
     28[[BR]][[BR]]
     29
     30== Conduction Front Simulations ==
     31The conduction front simulations can be seen here:[[BR]]
     32http://www.pas.rochester.edu/~shuleli/frame_0328.htm
     33[[BR]][[BR]]
     34More detailed results is summarized in the following paper:[[BR]]
     35Shule Li, Adam Frank, Eric Blackman, Astrophys Journal 748 (2012), 24-37
     36[[BR]][[BR]]
     37
    1938
    2039= Ablative RT in General =
    … …  
    4766density and temperature[[BR]]
    4867[[Image(http://www.pas.rochester.edu/~shuleli/densitycompare.png, 40%)]][[Image(http://www.pas.rochester.edu/~shuleli/tempcompare.png, 40%)]]
    49