| 1 | SUBROUTINE SFLUXI(PLEV,TLEV,DTAUI,TAUCUMI,UBARI,RSFI,WNOI,DWNI, |
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| 2 | * COSBI,WBARI,NFLUXTOPI,NFLUXTOPI_nu, |
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| 3 | * FMNETI,fluxupi,fluxdni,fluxupi_nu, |
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| 4 | * FZEROI,TAUGSURF) |
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| 5 | |
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| 6 | use radinc_h |
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| 7 | use radcommon_h, only: planckir, tlimit,sigma, gweight |
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| 8 | use comcstfi_mod, only: pi |
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| 9 | |
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| 10 | implicit none |
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| 11 | |
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| 12 | integer NLEVRAD, L, NW, NG, NTS, NTT |
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| 13 | |
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| 14 | real*8 TLEV(L_LEVELS), PLEV(L_LEVELS) |
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| 15 | real*8 TAUCUMI(L_LEVELS,L_NSPECTI,L_NGAUSS) |
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| 16 | real*8 FMNETI(L_NLAYRAD) |
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| 17 | real*8 WNOI(L_NSPECTI), DWNI(L_NSPECTI) |
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| 18 | real*8 DTAUI(L_NLAYRAD,L_NSPECTI,L_NGAUSS) |
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| 19 | real*8 FMUPI(L_NLEVRAD), FMDI(L_NLEVRAD) |
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| 20 | real*8 COSBI(L_NLAYRAD,L_NSPECTI,L_NGAUSS) |
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| 21 | real*8 WBARI(L_NLAYRAD,L_NSPECTI,L_NGAUSS) |
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| 22 | real*8 NFLUXTOPI |
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| 23 | real*8 NFLUXTOPI_nu(L_NSPECTI) |
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| 24 | real*8 fluxupi_nu(L_NLAYRAD,L_NSPECTI) |
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| 25 | real*8 FTOPUP |
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| 26 | |
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| 27 | real*8 UBARI, RSFI, TSURF, BSURF, TTOP, BTOP, TAUTOP |
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| 28 | real*8 PLANCK, PLTOP |
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| 29 | real*8 fluxupi(L_NLAYRAD), fluxdni(L_NLAYRAD) |
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| 30 | real*8 FZEROI(L_NSPECTI) |
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| 31 | real*8 taugsurf(L_NSPECTI,L_NGAUSS-1), fzero |
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| 32 | |
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| 33 | real*8 fup_tmp(L_NSPECTI),fdn_tmp(L_NSPECTI) |
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| 34 | real*8 PLANCKSUM,PLANCKREF |
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| 35 | |
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| 36 | ! AB : variables for interpolation |
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| 37 | REAL*8 C1 |
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| 38 | REAL*8 C2 |
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| 39 | REAL*8 P1 |
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| 40 | |
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| 41 | !======================================================================C |
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| 42 | |
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| 43 | NLEVRAD = L_NLEVRAD |
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| 44 | |
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| 45 | ! ZERO THE NET FLUXES |
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| 46 | NFLUXTOPI = 0.0D0 |
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| 47 | |
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| 48 | DO NW=1,L_NSPECTI |
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| 49 | NFLUXTOPI_nu(NW) = 0.0D0 |
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| 50 | DO L=1,L_NLAYRAD |
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| 51 | FLUXUPI_nu(L,NW) = 0.0D0 |
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| 52 | fup_tmp(nw)=0.0D0 |
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| 53 | fdn_tmp(nw)=0.0D0 |
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| 54 | END DO |
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| 55 | END DO |
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| 56 | |
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| 57 | DO L=1,L_NLAYRAD |
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| 58 | FMNETI(L) = 0.0D0 |
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| 59 | FLUXUPI(L) = 0.0D0 |
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| 60 | FLUXDNI(L) = 0.0D0 |
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| 61 | END DO |
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| 62 | |
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| 63 | ! WE NOW ENTER A MAJOR LOOP OVER SPECTRAL INTERVALS IN THE INFRARED |
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| 64 | ! TO CALCULATE THE NET FLUX IN EACH SPECTRAL INTERVAL |
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| 65 | |
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| 66 | TTOP = TLEV(2) ! JL12 why not (1) ??? |
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| 67 | TSURF = TLEV(L_LEVELS) |
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| 68 | |
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| 69 | NTS = int(TSURF*NTfac)-NTstart+1 |
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| 70 | NTT = int(TTOP *NTfac)-NTstart+1 |
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| 71 | |
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| 72 | !JL12 corrects the surface planck function so that its integral is equal to sigma Tsurf^4 |
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| 73 | !JL12 this ensure that no flux is lost due to: |
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| 74 | !JL12 -truncation of the planck function at high/low wavenumber |
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| 75 | !JL12 -numerical error during first spectral integration |
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| 76 | !JL12 -discrepancy between Tsurf and NTS/NTfac |
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| 77 | PLANCKSUM = 0.d0 |
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| 78 | PLANCKREF = TSURF * TSURF |
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| 79 | PLANCKREF = sigma * PLANCKREF * PLANCKREF |
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| 80 | |
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| 81 | DO NW=1,L_NSPECTI |
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| 82 | ! AB : PLANCKIR(NW,NTS) is replaced by P1, the linear interpolation result for a temperature TSURF |
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| 83 | C1 = TSURF * NTfac - int(TSURF * NTfac) |
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| 84 | P1 = (1.0D0 - C1) * PLANCKIR(NW,NTS) + C1 * PLANCKIR(NW,NTS+1) |
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| 85 | PLANCKSUM = PLANCKSUM + P1 * DWNI(NW) |
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| 86 | ENDDO |
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| 87 | |
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| 88 | PLANCKSUM = PLANCKREF / (PLANCKSUM * Pi) |
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| 89 | !JL12 |
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| 90 | |
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| 91 | DO 501 NW=1,L_NSPECTI |
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| 92 | ! SURFACE EMISSIONS - INDEPENDENT OF GAUSS POINTS |
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| 93 | ! AB : PLANCKIR(NW,NTS) is replaced by P1, the linear interpolation result for a temperature TSURF |
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| 94 | ! AB : idem for PLANCKIR(NW,NTT) and PLTOP |
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| 95 | C1 = TSURF * NTfac - int(TSURF * NTfac) |
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| 96 | C2 = TTOP * NTfac - int(TTOP * NTfac) |
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| 97 | P1 = (1.0D0 - C1) * PLANCKIR(NW,NTS) + C1 * PLANCKIR(NW,NTS+1) |
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| 98 | BSURF = (1. - RSFI) * P1 * PLANCKSUM |
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| 99 | PLTOP = (1.0D0 - C2) * PLANCKIR(NW,NTT) + C2*PLANCKIR(NW,NTT+1) |
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| 100 | |
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| 101 | ! If FZEROI(NW) = 1, then the k-coefficients are zero - skip to the |
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| 102 | ! special Gauss point at the end. |
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| 103 | FZERO = FZEROI(NW) |
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| 104 | |
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| 105 | IF(FZERO.ge.0.99) goto 40 |
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| 106 | |
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| 107 | DO NG=1,L_NGAUSS-1 |
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| 108 | |
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| 109 | if(TAUGSURF(NW,NG).lt. TLIMIT) then |
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| 110 | fzero = fzero + (1.0D0-FZEROI(NW))*GWEIGHT(NG) |
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| 111 | goto 30 |
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| 112 | end if |
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| 113 | |
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| 114 | ! SET UP THE UPPER AND LOWER BOUNDARY CONDITIONS ON THE IR |
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| 115 | ! CALCULATE THE DOWNWELLING RADIATION AT THE TOP OF THE MODEL |
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| 116 | ! OR THE TOP LAYER WILL COOL TO SPACE UNPHYSICALLY |
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| 117 | |
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| 118 | ! TAUTOP = DTAUI(1,NW,NG)*PLEV(2)/(PLEV(4)-PLEV(2)) |
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| 119 | TAUTOP = TAUCUMI(2,NW,NG) |
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| 120 | BTOP = (1.0D0-EXP(-TAUTOP/UBARI))*PLTOP |
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| 121 | |
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| 122 | ! WE CAN NOW SOLVE FOR THE COEFFICIENTS OF THE TWO STREAM |
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| 123 | ! CALL A SUBROUTINE THAT SOLVES FOR THE FLUX TERMS |
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| 124 | ! WITHIN EACH INTERVAL AT THE MIDPOINT WAVENUMBER |
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| 125 | |
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| 126 | CALL GFLUXI(NLEVRAD,TLEV,NW,DWNI(NW),DTAUI(1,NW,NG), |
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| 127 | * TAUCUMI(1,NW,NG), |
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| 128 | * WBARI(1,NW,NG),COSBI(1,NW,NG),UBARI,RSFI,BTOP, |
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| 129 | * BSURF,FTOPUP,FMUPI,FMDI) |
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| 130 | |
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| 131 | ! NOW CALCULATE THE CUMULATIVE IR NET FLUX |
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| 132 | NFLUXTOPI = NFLUXTOPI+FTOPUP*DWNI(NW)*GWEIGHT(NG) |
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| 133 | * * (1.0D0-FZEROI(NW)) |
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| 134 | |
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| 135 | ! and same thing by spectral band... (RDW) |
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| 136 | NFLUXTOPI_nu(NW) = NFLUXTOPI_nu(NW) + FTOPUP * DWNI(NW) |
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| 137 | * * GWEIGHT(NG) * (1.0D0-FZEROI(NW)) |
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| 138 | |
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| 139 | DO L=1,L_NLEVRAD-1 |
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| 140 | ! CORRECT FOR THE WAVENUMBER INTERVALS |
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| 141 | FMNETI(L) = FMNETI(L) + (FMUPI(L)-FMDI(L)) * DWNI(NW) |
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| 142 | * * GWEIGHT(NG)*(1.0D0-FZEROI(NW)) |
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| 143 | FLUXUPI(L) = FLUXUPI(L) + FMUPI(L)*DWNI(NW)*GWEIGHT(NG) |
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| 144 | * * (1.0D0-FZEROI(NW)) |
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| 145 | FLUXDNI(L) = FLUXDNI(L) + FMDI(L)*DWNI(NW)*GWEIGHT(NG) |
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| 146 | * * (1.0D0-FZEROI(NW)) |
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| 147 | ! and same thing by spectral band... (RW) |
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| 148 | FLUXUPI_nu(L,NW) = FLUXUPI_nu(L,NW) + FMUPI(L)*DWNI(NW) |
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| 149 | * * GWEIGHT(NG) * (1.0D0 - FZEROI(NW)) |
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| 150 | END DO |
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| 151 | |
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| 152 | 30 CONTINUE |
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| 153 | |
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| 154 | END DO !End NGAUSS LOOP |
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| 155 | |
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| 156 | 40 CONTINUE |
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| 157 | |
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| 158 | ! SPECIAL 17th Gauss point |
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| 159 | NG = L_NGAUSS |
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| 160 | |
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| 161 | ! TAUTOP = DTAUI(1,NW,NG)*PLEV(2)/(PLEV(4)-PLEV(2)) |
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| 162 | TAUTOP = TAUCUMI(2,NW,NG) |
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| 163 | BTOP = (1.0D0-EXP(-TAUTOP/UBARI))*PLTOP |
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| 164 | |
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| 165 | ! WE CAN NOW SOLVE FOR THE COEFFICIENTS OF THE TWO STREAM |
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| 166 | ! CALL A SUBROUTINE THAT SOLVES FOR THE FLUX TERMS |
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| 167 | ! WITHIN EACH INTERVAL AT THE MIDPOINT WAVENUMBER |
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| 168 | |
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| 169 | CALL GFLUXI(NLEVRAD,TLEV,NW,DWNI(NW),DTAUI(1,NW,NG), |
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| 170 | * TAUCUMI(1,NW,NG), |
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| 171 | * WBARI(1,NW,NG),COSBI(1,NW,NG),UBARI,RSFI,BTOP, |
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| 172 | * BSURF,FTOPUP,FMUPI,FMDI) |
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| 173 | |
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| 174 | ! NOW CALCULATE THE CUMULATIVE IR NET FLUX |
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| 175 | NFLUXTOPI = NFLUXTOPI+FTOPUP*DWNI(NW)*FZERO |
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| 176 | |
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| 177 | ! and same thing by spectral band... (RW) |
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| 178 | NFLUXTOPI_nu(NW) = NFLUXTOPI_nu(NW) |
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| 179 | * +FTOPUP*DWNI(NW)*FZERO |
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| 180 | |
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| 181 | DO L=1,L_NLEVRAD-1 |
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| 182 | ! CORRECT FOR THE WAVENUMBER INTERVALS |
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| 183 | FMNETI(L) = FMNETI(L)+(FMUPI(L)-FMDI(L))*DWNI(NW)*FZERO |
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| 184 | FLUXUPI(L) = FLUXUPI(L) + FMUPI(L)*DWNI(NW)*FZERO |
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| 185 | FLUXDNI(L) = FLUXDNI(L) + FMDI(L)*DWNI(NW)*FZERO |
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| 186 | ! and same thing by spectral band... (RW) |
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| 187 | FLUXUPI_nu(L,NW) = FLUXUPI_nu(L,NW) |
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| 188 | * + FMUPI(L) * DWNI(NW) * FZERO |
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| 189 | END DO |
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| 190 | |
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| 191 | 501 CONTINUE !End Spectral Interval LOOP |
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| 192 | ! *** END OF MAJOR SPECTRAL INTERVAL LOOP IN THE INFRARED**** |
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| 193 | |
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| 194 | RETURN |
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| 195 | END |
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