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WRF Model: Physics Implementation

P. F. I. H. R. C. Y. W. S. S. WRF Model: Physics Implementation. Shu-hua Chen NCAR/AFWA (UC Davis, Sep.). OUTLINE. Physics Schemes Three_level Structure Rules for WRF physics WRF Physics Features WRF Language What you might need to do. P. F. I. H. R. C. Y. W. S. S.

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WRF Model: Physics Implementation

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  1. P F I H R C Y W S S WRF Model: Physics Implementation Shu-hua Chen NCAR/AFWA (UC Davis, Sep.) OUTLINE Physics Schemes Three_level Structure Rules for WRF physics WRF Physics Features WRF Language What you might need to do

  2. P F I H R C Y W S S Scheme Selection Simple schemes for operation Complicated schemes for research

  3. P F I H R C Y W S S Physics Schemes Physical Process Available Microphysics Kessler, Lin et al. , Ncloud3, Ncloud5 Cumulus KF, BMJ Subgrid scale turbulence TKE, Smagrinsky, Constant K Radiation RRTM(L), Dudhia(S), Goddard(S) PBL MRF Surface layer Similarity theory Land-surface layer 5-layer soil temperature

  4. P F I H R C Y W S S • User friendly • Different dynamics cores • Simple Three-level structure => Physics Interface Design

  5. P F I H R C Y W S S Solver Physics_driver SELECT CASE (CHOICE) CASE ( NOPHY ) CASE( SCHEME1 ) CALL XXX CASE( SCHEME2 ) CALL YYY . CASE DEFAULT END SELECT Individual physics scheme ( XXX ) Three-level Structure

  6. P F I R H C W Y S S phy_prep phy_init Radiation_driver pbl_driver Cumulus_driver moist_physics_prep microphysics_driver … INIT . WRF solve_rk … ADV TENDENCIES . ADVANCE VARS .

  7. P F I H R C Y W S S phy_prep & moist_physics_prep • Decouple variables • Convert variables from C grid to A grid

  8. P F I H R C Y W S S Solver Physics_driver SELECT CASE (CHOICE) CASE ( NOPHY ) CASE( SCHEME1 ) CALL XXX CASE( SCHEME2 ) CALL YYY . CASE DEFAULT END SELECT Individual physics scheme ( XXX ) Three-level Structure

  9. P F I H R C Y W S S Physics_driver SELECT CASE (CHOICE) CASE ( NOPHY ) CASE( SCHEME1 ) CALL XXX(…) CASE( SCHEME2 ) CALL YYY(…) . CASE DEFAULT END SELECT Physics Standard Interface

  10. P F I H R C Y W S S Solver Physics_driver SELECT CASE (CHOICE) CASE ( NOPHY ) CASE( SCHEME1 ) CALL XXX CASE( SCHEME2 ) CALL YYY . CASE DEFAULT END SELECT Individual physics scheme ( XXX ) Three-level Structure

  11. P F I H R C Y W S S Three Sets of Dimensions Domain size: ids, ide, jds, jde, kds, kde Memory size: ims, ime, jms, jme, kms, kme Tile size: its, ite, jts, jte, kts, kte

  12. P F I H R C Y W S S (ids,ide) Logical Domain (ids,kds,jds)

  13. P F I H R C Y W S S patch patch patch halo halo patch patch halo patch halo (ims,ime) patch patch patch (ids,ide) Memory size (ims,kms,jms)

  14. P F I H R C Y W S S halo tile tile tile halo halo (its,ite) tile tile tile halo (ims,ime) Tile size (its,kts,jds)

  15. P F I R H C W Y S S phy_prep phy_init Radiation_driver pbl_driver Cumulus_driver moist_physics_prep microphysics_driver … INIT . WRF solve_rk … ADV TENDENCIES . ADVANCE VARS .

  16. P F I H R C Y W S S Rules for WRF Physics • Coding rules

  17. P F I H R C Y W S S F77 Subroutine kessler(QV, T, & its,ite,jts,jte,kts,kte, & ims,ime,jms,jme,kms,kme, & ids,ide,jds,jde,kds,kde) F90 Subroutine kessler(QV, T, . . . & its,ite,jts,jte,kts,kte,& ims,ime,jms,jme,kms,kme,& ids,ide,jds,jde,kds,kde ) Coding Rules 1. F90 • Replace continuation characters in the 6th column with f90 continuation `&‘ at end of previous line

  18. P F I H R C Y W S S F77 c This is a test F90 ! This is a test Coding Rules 1. F90 • Replace continuation characters in the 6th column with f90 continuation `&‘ at end of previous line b)Replace the 1st column `C` for comment with `!`

  19. P F I H R C Y W S S Coding Rules 1. F90 • Replace continuation characters in the 6th column with f90 continuation `&‘ at end of previous line b)Replace the 1st column `C` for comment with `!` 2. No common block 3. Use “ implicit none ” 4. Use “ intent ” 5. Variable dimensions and do loops

  20. P F I H R C Y W S S Rules for WRF Physics • Coding rules • One scheme one module • Naming rules

  21. P F I H R C Y W S S Naming Rules module_yy_xxx.F(module) yy = ra is for radiation bl is for PBL cu is for cumulus mp is for microphysics. xxx = individual scheme ex, module_cu_kf.F

  22. P F I H R C Y W S S Naming Rules RXXYYTEN(tendencies) XX = variable (th, u, v, qv, qc, … ) YY = ra is for radiation bl is for PBL cu is for cumulus ex, RTHBLTEN

  23. P F I H R C Y W S S Rules for WRF Physics • Coding rules • One scheme one module • Naming rules • Vectorized code preferred ( might depend on which physics component )

  24. P F I H R C Y W S S REAL , PARAMETER :: r_d = 287. REAL , PARAMETER :: r_v = 461.6 REAL , PARAMETER :: cp = 7.*r_d/2. REAL , PARAMETER :: cv = cp-r_d . . . WRF Physics Features • Unified global constatnts (module_model_constants.F)

  25. P F I H R C Y W S S WRF Physics Features • Unified global constatnts (module_model_constants.F) • Unified common calculations (saturation mixing ratio) • Vertical index (kms is at the bottom)

  26. P F I H R C Y W S S Solver Physics_driver SELECT CASE (CHOICE) CASE ( NOPHY ) CASE( SCHEME1 ) CALL XXX CASE( SCHEME2 ) CALL YYY . CASE DEFAULT END SELECT Individual physics scheme ( XXX ) Three-level Structure

  27. P F I H R C Y W S S WRF Physics Features • Unified global constatnts (module_model_constants.F) • Unified common calculations (saturation mixing ratio) • Vertical index (kms is at bottom) • kme = kte + 1 (physics) kme = kte (dynamics)

  28. P F I H R C Y W S S WRF Language • Patch, tile, …. • Moisture field, moist(i,k,j,?), is 4D • ? = P_QV, P_QC, P_QR, P_QI,P_QS, P_QG (module_state_description.F) • PARAM_FIRST_SCALAR IF ( P_QI .ge. PARAM_FIRST_SCALAR ) . . .

  29. P F I H R C Y W S S package kesslerscheme mp_physics==1 - moist:qv,qc,qr package linscheme mp_physics==2 - moist:qv,qc,qr,qi,qs,qg package ncepcloud3 mp_physics==3 - moist:qv,qc,qr package ncepcloud5 mp_physics==4 - moist:qv,qc, P_QV, P_QC, P_QR, … Registry

  30. P F I H R C Y W S S Physics Buffet (namelist.input) mp_physics = 2, ra_lw_physics = 1, ra_sw_physics = 1, bl_sfclay_physics = 1, bl_surface_physics = 1, bl_pbl_physics = 1, cu_physics = 1, What you might need to do ? • Run existing codes

  31. P F I H R C Y W S S What you might need to do ? • Run existing codes • Modify existing codes • Plug in your own codes

  32. P F I H R C Y W S S WRF Development Team

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