absorb

absorb

frei.absorb(opacities, temperatures, pressures, lam, F_TOA, g, m_bar=<Quantity 4.01429262e-27 kg>, n_timesteps=50, convergence_thresh=<Quantity 10. K>, alpha=1, fluxes_up=None, fluxes_down=None)[source]

Compute emission spectrum.

Parameters
  • opacities (dict) – Opacity database binned to wavelength grid.

  • temperatures (Quantity) – Temperature grid

  • pressures (Quantity) – Pressure grid

  • lam (Quantity) – Wavelength grid

  • F_TOA (Quantity) – Flux at the top of the atmosphere

  • g (Quantity) – Surface graivty

  • m_bar (Quantity) – Mean molecular weight

  • n_timesteps (int) – Maximum number of timesteps in iteration for radiative equilibrium

  • convergence_thresh (Quantity) – When the maximum change in temperature between timesteps is less than convergence_thresh, accept this timestep as “converged”.

Returns

  • F_2_up (~astropy.units.Quantity) – Outgoing flux

  • final_temps (~astropy.units.Quantity) – Final temperature grid

  • temperature_history (~astropy.units.Quantity) – Grid of temperatures with dimensions (n_layers, n_timesteps)

  • dtaus (~numpy.ndarray) – Change in optical depth in final iteration