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Primary variables

M_p R_p T_p \rho_p M_s R_s T_s \rho_s a

Equations

• \chi = \rho_p / \rho_s
• \lambda_p=\frac{G M_p m_H}{R_p k_b T_p}
• \lambda_s=\frac{G M_s m_H}{R_s k_b T_s}
• \omega = \sqrt{\frac{G \left (M_s+M_p \right )}{a^3}}
• r_H=a \left (\frac{M_p}{3M_s} \right )^{1/3}

Planetary Atmospheres

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
• Source code problem.f90​
• Data file problem.data​
• Uses Particles, Ambients, Clumps, and Refinement Objects

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)

Results

Working on getting stable planetary atmosphere using profile without a core. Turning on characteristic limiting seems to cause numerical artifacts which lead to 'explosion'. See ticket #