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intercomparisons:c3_cumulus
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intercomparisons:c3_cumulus [2016/11/16 21:28] claudia [Detailed plots for all models, pure molecular atmosphere] |
intercomparisons:c3_cumulus [2016/11/16 21:47] claudia [Results for pure Rayleigh background atmospehre] |
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| //Setup:// | //Setup:// | ||
| - | * Cumulus cloud field from LES model (same as used in I3RC project, $r_{eff}$ depending on LWC): | + | * Cumulus cloud field from LES model (same as used in I3RC project, $r_{\rm eff}$ depending on LWC): |
| {{:intercomparisons:phase_c:cumulus.dat}}, the format of the ascii file is as follows: | {{:intercomparisons:phase_c:cumulus.dat}}, the format of the ascii file is as follows: | ||
| Nx Ny Nz flag | Nx Ny Nz flag | ||
| Line 91: | Line 91: | ||
| * Stokes component U (third row): Also for U, there are systematic differences between SPARTA and other Monte Carlo models for cases 2 and 3. | * Stokes component U (third row): Also for U, there are systematic differences between SPARTA and other Monte Carlo models for cases 2 and 3. | ||
| * Stokes component V (bottom row): Mean radiance for V is dominated by noise, so here we can not compare the models quantitatively. | * Stokes component V (bottom row): Mean radiance for V is dominated by noise, so here we can not compare the models quantitatively. | ||
| - | * Generally the standard deviation for SPARTA is below 3DMCPOL because for SPARTA more photons were used (10e11 vs. 49e9). MYSTIC and MSCART used 49e9 photons and variance reduction techniques which decrease the standard deviation approximately by almost one order of magnitude. | + | |
| ==== Results with atmosphere ==== | ==== Results with atmosphere ==== | ||
intercomparisons/c3_cumulus.txt ยท Last modified: 2018/01/08 12:23 (external edit)
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