Meeting Update 0814 - Jason and Ivan

We are heading towards an hydrostatic equilibrium solution.
There are 2 possible approaches, we are currently evaluating the best path to follow.

* Scenario 1 (Manual density profile):

User defined variables: density profile ⇒ rho0*(r/r0)-2
Pressure would be calculated accordingly by the hydrostatic equation.
Temperature can be changed by adjusting the density profile.

Pros:

  • Is the classic implementation of the hydrostatic equilibrium
  • Density profile is consistent with AGB stars models

Cons:

  • P(r) involves integral calculation
  • Scarce usage of astrobear functions, introduces a window for errors
  • Temperature profile could not be what we want for our type of simulations

* Scenario 2 (Isothermal profile, suggested by Jonathan):

User defined variables: constant ratio (pressure/rho)
Pressure and density would be calculated accordingly

Pros:

  • Usage of astrobear common functions, less possbility of errors
  • Does not involve manual calculation of integrals
  • Gives us the temperature profile that we need

Cons:

  • Density profile could not be disk friendly

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