| Version 6 (modified by , 11 years ago) ( diff ) |
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Planetary Atmospheres
Description of Problem
Hot Jupiters receive much more energy through stellar irradiation then internal heating. They are also tidally locked due to their proximity. Dayside at 1000K, night side at 100K without heat redistribution.
Profiles
- Density
- Enclosed Mass
- Pressure - and rho*R*T mismatch
Module supports
- Global simulation in a fixed frame
- Global simulation in a rotating frame
- Local simulation in a rotating frame
- Spatial based Refinement of planet
- Stellar envelope in HSE
Still working on
- Basic testing of hydrostatic equilibrium for planet
- Line transfer for stellar heating
- Second AMR implicit solve may need to be added later (ie Howell and Greenough 2002)
Attachments (13)
- Limiter.png (28.1 KB ) - added by 11 years ago.
- Screen Shot 2013-10-02 at 9.04.53 AM.png (44.9 KB ) - added by 11 years ago.
- Screen Shot 2013-10-02 at 9.06.06 AM.png (140.9 KB ) - added by 11 years ago.
- Screen Shot 2013-10-02 at 9.08.08 AM.png (175.4 KB ) - added by 11 years ago.
- Screen Shot 2013-10-02 at 10.12.16 AM.png (77.3 KB ) - added by 11 years ago.
- Screen Shot 2013-10-02 at 2.33.57 PM.png (43.8 KB ) - added by 11 years ago.
- Screen Shot 2013-10-02 at 2.33.42 PM.png (48.8 KB ) - added by 11 years ago.
- Screen Shot 2013-10-02 at 10.12.16 AM.2.png (77.3 KB ) - added by 11 years ago.
- problem.f90 (8.4 KB ) - added by 11 years ago.
- problem.data (735 bytes ) - added by 11 years ago.
- calcvars.m (2.7 KB ) - added by 9 years ago.
- mypsi.m (156 bytes ) - added by 9 years ago.
- phi.m (72 bytes ) - added by 9 years ago.
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