| 1 | SUBROUTINE OPTCV(DTAUV,TAUV,TAUCUMV,PLEV, & |
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| 2 | QXVAER,QSVAER,GVAER,WBARV,COSBV, & |
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| 3 | TAURAY,TAUAERO,TMID,PMID,TAUGSURF) |
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| 4 | |
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| 5 | use radinc_h |
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| 6 | use radcommon_h, only: gasv, tlimit, Cmk, tgasref, pfgasref,wnov,scalep,indv,glat_ig,gweight |
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| 7 | use gases_h |
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| 8 | use comcstfi_mod, only: g, r |
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| 9 | use callkeys_mod, only: continuum,graybody,callgasvis |
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| 10 | |
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| 11 | implicit none |
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| 12 | |
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| 13 | !================================================================== |
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| 14 | ! |
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| 15 | ! Purpose |
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| 16 | ! ------- |
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| 17 | ! Calculates shortwave optical constants at each level. |
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| 18 | ! |
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| 19 | ! Authors |
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| 20 | ! ------- |
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| 21 | ! Adapted from the NASA Ames code by R. Wordsworth (2009) |
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| 22 | ! |
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| 23 | !================================================================== |
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| 24 | ! |
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| 25 | ! THIS SUBROUTINE SETS THE OPTICAL CONSTANTS IN THE VISUAL |
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| 26 | ! IT CALCULATES FOR EACH LAYER, FOR EACH SPECTRAL INTERVAL IN THE VISUAL |
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| 27 | ! LAYER: WBAR, DTAU, COSBAR |
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| 28 | ! LEVEL: TAU |
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| 29 | ! |
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| 30 | ! TAUV(L,NW,NG) is the cumulative optical depth at the top of radiation code |
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| 31 | ! layer L. NW is spectral wavelength interval, ng the Gauss point index. |
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| 32 | ! |
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| 33 | ! TLEV(L) - Temperature at the layer boundary |
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| 34 | ! PLEV(L) - Pressure at the layer boundary (i.e. level) |
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| 35 | ! GASV(NT,NPS,NW,NG) - Visible k-coefficients |
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| 36 | ! |
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| 37 | !------------------------------------------------------------------- |
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| 38 | |
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| 39 | |
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| 40 | real*8 DTAUV(L_NLAYRAD,L_NSPECTV,L_NGAUSS) |
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| 41 | real*8 DTAUKV(L_LEVELS,L_NSPECTV,L_NGAUSS) |
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| 42 | real*8 TAUV(L_NLEVRAD,L_NSPECTV,L_NGAUSS) |
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| 43 | real*8 TAUCUMV(L_LEVELS,L_NSPECTV,L_NGAUSS) |
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| 44 | real*8 PLEV(L_LEVELS) |
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| 45 | real*8 TMID(L_LEVELS), PMID(L_LEVELS) |
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| 46 | real*8 COSBV(L_NLAYRAD,L_NSPECTV,L_NGAUSS) |
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| 47 | real*8 WBARV(L_NLAYRAD,L_NSPECTV,L_NGAUSS) |
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| 48 | |
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| 49 | ! for aerosols |
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| 50 | real*8 QXVAER(L_LEVELS,L_NSPECTV,NAERKIND) |
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| 51 | real*8 QSVAER(L_LEVELS,L_NSPECTV,NAERKIND) |
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| 52 | real*8 GVAER(L_LEVELS,L_NSPECTV,NAERKIND) |
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| 53 | real*8 TAUAERO(L_LEVELS,NAERKIND) |
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| 54 | real*8 TAUAEROLK(L_LEVELS,L_NSPECTV,NAERKIND) |
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| 55 | real*8 TAEROS(L_LEVELS,L_NSPECTV,NAERKIND) |
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| 56 | |
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| 57 | ! Titan customisation |
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| 58 | ! J. Vatant d'Ollone (2016) |
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| 59 | real*8 DHAZE_T(L_LEVELS,L_NSPECTI) |
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| 60 | real*8 DHAZES_T(L_LEVELS,L_NSPECTI) |
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| 61 | real*8 SSA_T(L_LEVELS,L_NSPECTI) |
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| 62 | real*8 ASF_T(L_LEVELS,L_NSPECTI) |
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| 63 | real*8 INT_DTAU(L_NLAYRAD,L_NSPECTI) |
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| 64 | real*8 K_HAZE(L_NLAYRAD,L_NSPECTI) |
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| 65 | |
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| 66 | CHARACTER*2 str2 |
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| 67 | ! ========================== |
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| 68 | |
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| 69 | integer L, NW, NG, K, LK, IAER |
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| 70 | integer MT(L_LEVELS), MP(L_LEVELS), NP(L_LEVELS) |
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| 71 | real*8 ANS, TAUGAS |
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| 72 | real*8 TAURAY(L_NSPECTV) |
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| 73 | real*8 TRAY(L_LEVELS,L_NSPECTV) |
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| 74 | real*8 DPR(L_LEVELS), U(L_LEVELS) |
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| 75 | real*8 LCOEF(4), LKCOEF(L_LEVELS,4) |
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| 76 | |
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| 77 | real*8 taugsurf(L_NSPECTV,L_NGAUSS-1) |
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| 78 | real*8 DCONT,DAERO |
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| 79 | real*8 DRAYAER |
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| 80 | double precision wn_cont, p_cont, p_air, T_cont, dtemp, dtempc |
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| 81 | double precision p_cross |
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| 82 | |
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| 83 | real*8 KCOEF(4) |
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| 84 | |
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| 85 | ! temporary variable to reduce memory access time to gasv |
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| 86 | real*8 tmpk(2,2) |
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| 87 | |
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| 88 | ! temporary variables for multiple aerosol calculation |
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| 89 | real*8 atemp(L_NLAYRAD,L_NSPECTV) |
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| 90 | real*8 btemp(L_NLAYRAD,L_NSPECTV) |
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| 91 | real*8 ctemp(L_NLAYRAD,L_NSPECTV) |
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| 92 | |
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| 93 | ! variables for k in units m^-1 |
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| 94 | real*8 dz(L_LEVELS) |
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| 95 | |
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| 96 | integer igas, jgas, ilay |
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| 97 | |
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| 98 | integer interm |
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| 99 | |
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| 100 | !! AS: to save time in computing continuum (see bilinearbig) |
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| 101 | IF (.not.ALLOCATED(indv)) THEN |
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| 102 | ALLOCATE(indv(L_NSPECTV,ngasmx,ngasmx)) |
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| 103 | indv = -9999 ! this initial value means "to be calculated" |
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| 104 | ENDIF |
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| 105 | |
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| 106 | !======================================================================= |
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| 107 | ! Determine the total gas opacity throughout the column, for each |
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| 108 | ! spectral interval, NW, and each Gauss point, NG. |
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| 109 | ! Calculate the continuum opacities, i.e., those that do not depend on |
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| 110 | ! NG, the Gauss index. |
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| 111 | |
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| 112 | taugsurf(:,:) = 0.0 |
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| 113 | dpr(:) = 0.0 |
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| 114 | lkcoef(:,:) = 0.0 |
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| 115 | |
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| 116 | do K=2,L_LEVELS |
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| 117 | DPR(k) = PLEV(K)-PLEV(K-1) |
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| 118 | |
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| 119 | ! if we have continuum opacities, we need dz |
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| 120 | |
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| 121 | dz(k) = dpr(k)*R*TMID(K)/(glat_ig*PMID(K)) |
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| 122 | U(k) = Cmk*DPR(k) ! only Cmk line in optcv.F |
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| 123 | |
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| 124 | call tpindex(PMID(K),TMID(K),pfgasref,tgasref,LCOEF,MT(K),MP(K)) |
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| 125 | |
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| 126 | do LK=1,4 |
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| 127 | LKCOEF(K,LK) = LCOEF(LK) |
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| 128 | end do |
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| 129 | end do ! levels |
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| 130 | |
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| 131 | ! Spectral dependance of aerosol absorption |
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| 132 | do iaer=1,naerkind |
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| 133 | do NW=1,L_NSPECTV |
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| 134 | do K=2,L_LEVELS |
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| 135 | TAEROS(K,NW,IAER) = TAUAERO(K,IAER) * QXVAER(K,NW,IAER) |
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| 136 | end do ! levels |
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| 137 | end do |
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| 138 | end do |
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| 139 | |
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| 140 | ! Rayleigh scattering |
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| 141 | do NW=1,L_NSPECTV |
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| 142 | do K=2,L_LEVELS |
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| 143 | TRAY(K,NW) = TAURAY(NW) * DPR(K) |
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| 144 | end do ! levels |
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| 145 | end do |
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| 146 | |
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| 147 | ! we ignore K=1... |
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| 148 | do K=2,L_LEVELS |
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| 149 | |
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| 150 | ilay = k / 2 ! int. arithmetic => gives the gcm layer index |
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| 151 | |
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| 152 | do NW=1,L_NSPECTV |
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| 153 | |
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| 154 | !================= Titan customisation ======================================== |
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| 155 | call disr_haze(dz(k),plev(k),wnov(nw),dhaze_T(k,nw),SSA_T(k,nw),ASF_T(k,nw)) |
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| 156 | ! ============================================================================= |
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| 157 | |
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| 158 | DRAYAER = TRAY(K,NW) |
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| 159 | ! DRAYAER is Tau RAYleigh scattering, plus AERosol opacity |
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| 160 | do iaer=1,naerkind |
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| 161 | DRAYAER = DRAYAER + TAEROS(K,NW,IAER) |
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| 162 | end do |
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| 163 | |
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| 164 | DRAYAER = DRAYAER + DHAZE_T(K,NW) ! Titan's aerosol |
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| 165 | |
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| 166 | DCONT = 0.0 ! continuum absorption |
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| 167 | |
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| 168 | if(continuum.and.(.not.graybody).and.callgasvis)then |
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| 169 | ! include continua if necessary |
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| 170 | wn_cont = dble(wnov(nw)) |
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| 171 | T_cont = dble(TMID(k)) |
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| 172 | do igas=1,ngasmx |
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| 173 | |
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| 174 | p_cont = dble(PMID(k)*scalep*gfrac(igas,ilay)) |
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| 175 | |
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| 176 | dtemp=0.0 |
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| 177 | if(igas.eq.igas_N2)then |
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| 178 | |
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| 179 | interm = indv(nw,igas,igas) |
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| 180 | ! call interpolateN2N2(wn_cont,T_cont,p_cont,dtemp,.false.,interm) |
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| 181 | indv(nw,igas,igas) = interm |
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| 182 | ! only goes to 500 cm^-1, so unless we're around a cold brown dwarf, this is irrelevant in the visible |
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| 183 | |
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| 184 | elseif(igas.eq.igas_H2)then |
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| 185 | |
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| 186 | ! first do self-induced absorption |
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| 187 | interm = indv(nw,igas,igas) |
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| 188 | call interpolateH2H2(wn_cont,T_cont,p_cont,dtemp,.false.,interm) |
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| 189 | indv(nw,igas,igas) = interm |
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| 190 | |
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| 191 | ! then cross-interactions with other gases |
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| 192 | do jgas=1,ngasmx |
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| 193 | p_cross = dble(PMID(k)*scalep*gfrac(jgas,ilay)) |
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| 194 | dtempc = 0.0 |
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| 195 | if(jgas.eq.igas_N2)then |
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| 196 | interm = indv(nw,igas,jgas) |
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| 197 | call interpolateN2H2(wn_cont,T_cont,p_cross,p_cont,dtempc,.false.,interm) |
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| 198 | indv(nw,igas,jgas) = interm |
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| 199 | ! should be irrelevant in the visible |
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| 200 | endif |
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| 201 | dtemp = dtemp + dtempc |
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| 202 | enddo |
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| 203 | |
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| 204 | elseif(igas.eq.igas_CH4)then |
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| 205 | |
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| 206 | ! first do self-induced absorption |
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| 207 | interm = indv(nw,igas,igas) |
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| 208 | call interpolateCH4CH4(wn_cont,T_cont,p_cont,dtemp,.false.,interm) |
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| 209 | indv(nw,igas,igas) = interm |
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| 210 | |
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| 211 | ! then cross-interactions with other gases |
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| 212 | do jgas=1,ngasmx |
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| 213 | p_cross = dble(PMID(k)*scalep*gfrac(jgas,ilay)) |
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| 214 | dtempc = 0.0 |
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| 215 | if(jgas.eq.igas_N2)then |
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| 216 | interm = indv(nw,igas,jgas) |
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| 217 | call interpolateN2CH4(wn_cont,T_cont,p_cross,p_cont,dtempc,.false.,interm) |
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| 218 | indv(nw,igas,jgas) = interm |
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| 219 | endif |
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| 220 | dtemp = dtemp + dtempc |
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| 221 | enddo |
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| 222 | |
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| 223 | endif |
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| 224 | |
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| 225 | DCONT = DCONT + dtemp |
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| 226 | |
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| 227 | enddo |
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| 228 | |
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| 229 | DCONT = DCONT*dz(k) |
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| 230 | |
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| 231 | endif |
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| 232 | |
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| 233 | do ng=1,L_NGAUSS-1 |
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| 234 | |
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| 235 | ! Now compute TAUGAS |
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| 236 | |
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| 237 | ! JVO 2017 : added tmpk because the repeated calls to gasi/v increased dramatically |
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| 238 | ! the execution time of optci/v -> ~ factor 2 on the whole radiative |
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| 239 | ! transfer on the tested simulations ! |
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| 240 | |
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| 241 | tmpk = GASV(MT(K):MT(K)+1,MP(K):MP(K)+1,1,NW,NG) |
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| 242 | |
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| 243 | KCOEF(1) = tmpk(1,1) ! KCOEF(1) = GASV(MT(K),MP(K),1,NW,NG) |
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| 244 | KCOEF(2) = tmpk(1,2) ! KCOEF(2) = GASV(MT(K),MP(K)+1,1,NW,NG) |
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| 245 | KCOEF(3) = tmpk(2,2) ! KCOEF(3) = GASV(MT(K)+1,MP(K)+1,1,NW,NG) |
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| 246 | KCOEF(4) = tmpk(2,1) ! KCOEF(4) = GASV(MT(K)+1,MP(K),1,NW,NG) |
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| 247 | |
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| 248 | ! Interpolate the gaseous k-coefficients to the requested T,P values |
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| 249 | |
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| 250 | ANS = LKCOEF(K,1)*KCOEF(1) + LKCOEF(K,2)*KCOEF(2) + & |
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| 251 | LKCOEF(K,3)*KCOEF(3) + LKCOEF(K,4)*KCOEF(4) |
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| 252 | |
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| 253 | |
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| 254 | TAUGAS = U(k)*ANS |
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| 255 | |
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| 256 | TAUGSURF(NW,NG) = TAUGSURF(NW,NG) + TAUGAS + DCONT |
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| 257 | DTAUKV(K,nw,ng) = TAUGAS & |
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| 258 | + DRAYAER & ! DRAYAER includes all scattering contributions |
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| 259 | + DCONT ! For parameterized continuum aborption |
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| 260 | |
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| 261 | end do |
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| 262 | |
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| 263 | ! Now fill in the "clear" part of the spectrum (NG = L_NGAUSS), |
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| 264 | ! which holds continuum opacity only |
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| 265 | |
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| 266 | NG = L_NGAUSS |
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| 267 | DTAUKV(K,nw,ng) = DRAYAER + DCONT ! Scattering + parameterized continuum absorption, including Titan's haze |
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| 268 | |
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| 269 | end do |
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| 270 | end do |
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| 271 | |
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| 272 | |
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| 273 | !======================================================================= |
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| 274 | ! Now the full treatment for the layers, where besides the opacity |
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| 275 | ! we need to calculate the scattering albedo and asymmetry factors |
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| 276 | |
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| 277 | do iaer=1,naerkind |
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| 278 | DO NW=1,L_NSPECTV |
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| 279 | DO K=2,L_LEVELS |
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| 280 | TAUAEROLK(K,NW,IAER) = TAUAERO(K,IAER) * QSVAER(K,NW,IAER) ! effect of scattering albedo |
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| 281 | ENDDO |
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| 282 | ENDDO |
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| 283 | end do |
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| 284 | |
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| 285 | ! Haze scattering |
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| 286 | DO NW=1,L_NSPECTV |
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| 287 | DO K=2,L_LEVELS |
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| 288 | DHAZES_T(K,NW) = DHAZE_T(K,NW) * SSA_T(K,NW) ! effect of scattering albedo on haze |
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| 289 | ENDDO |
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| 290 | ENDDO |
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| 291 | |
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| 292 | |
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| 293 | DO NW=1,L_NSPECTV |
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| 294 | DO L=1,L_NLAYRAD-1 |
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| 295 | K = 2*L+1 |
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| 296 | atemp(L,NW) = SUM(GVAER(K,NW,1:naerkind) * TAUAEROLK(K,NW,1:naerkind))+SUM(GVAER(K+1,NW,1:naerkind) * TAUAEROLK(K+1,NW,1:naerkind)) & |
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| 297 | + ASF_T(K,NW)*DHAZES_T(K,NW) + ASF_T(K+1,NW)*DHAZES_T(K+1,NW) |
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| 298 | btemp(L,NW) = SUM(TAUAEROLK(K,NW,1:naerkind)) + SUM(TAUAEROLK(K+1,NW,1:naerkind)) & |
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| 299 | + DHAZES_T(K,NW) + DHAZES_T(K+1,NW) |
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| 300 | ctemp(L,NW) = btemp(L,NW) + 0.9999*(TRAY(K,NW) + TRAY(K+1,NW)) ! JVO 2017 : does this 0.999 is really meaningful ? |
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| 301 | btemp(L,NW) = btemp(L,NW) + TRAY(K,NW) + TRAY(K+1,NW) |
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| 302 | COSBV(L,NW,1:L_NGAUSS) = atemp(L,NW)/btemp(L,NW) |
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| 303 | END DO ! L vertical loop |
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| 304 | |
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| 305 | ! Last level |
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| 306 | L = L_NLAYRAD |
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| 307 | K = 2*L+1 |
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| 308 | atemp(L,NW) = SUM(GVAER(K,NW,1:naerkind) * TAUAEROLK(K,NW,1:naerkind)) & |
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| 309 | + ASF_T(K,NW)*DHAZES_T(K,NW) |
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| 310 | btemp(L,NW) = SUM(TAUAEROLK(K,NW,1:naerkind)) & |
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| 311 | + DHAZES_T(K,NW) |
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| 312 | ctemp(L,NW) = btemp(L,NW) + 0.9999*TRAY(K,NW) ! JVO 2017 : does this 0.999 is really meaningful ? |
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| 313 | btemp(L,NW) = btemp(L,NW) + TRAY(K,NW) |
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| 314 | COSBV(L,NW,1:L_NGAUSS) = atemp(L,NW)/btemp(L,NW) |
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| 315 | |
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| 316 | |
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| 317 | END DO ! NW spectral loop |
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| 318 | |
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| 319 | DO NG=1,L_NGAUSS |
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| 320 | DO NW=1,L_NSPECTV |
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| 321 | DO L=1,L_NLAYRAD-1 |
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| 322 | |
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| 323 | K = 2*L+1 |
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| 324 | DTAUV(L,nw,ng) = DTAUKV(K,NW,NG) + DTAUKV(K+1,NW,NG) |
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| 325 | WBARV(L,nw,ng) = ctemp(L,NW) / DTAUV(L,nw,ng) |
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| 326 | |
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| 327 | END DO ! L vertical loop |
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| 328 | |
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| 329 | ! Last level |
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| 330 | |
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| 331 | L = L_NLAYRAD |
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| 332 | K = 2*L+1 |
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| 333 | DTAUV(L,nw,ng) = DTAUKV(K,NW,NG) |
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| 334 | |
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| 335 | WBARV(L,NW,NG) = ctemp(L,NW) / DTAUV(L,NW,NG) |
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| 336 | |
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| 337 | END DO ! NW spectral loop |
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| 338 | END DO ! NG Gauss loop |
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| 339 | |
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| 340 | ! Total extinction optical depths |
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| 341 | |
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| 342 | DO NG=1,L_NGAUSS ! full gauss loop |
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| 343 | DO NW=1,L_NSPECTV |
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| 344 | TAUV(1,NW,NG)=0.0D0 |
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| 345 | DO L=1,L_NLAYRAD |
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| 346 | TAUV(L+1,NW,NG)=TAUV(L,NW,NG)+DTAUV(L,NW,NG) |
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| 347 | END DO |
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| 348 | |
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| 349 | TAUCUMV(1,NW,NG)=0.0D0 |
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| 350 | DO K=2,L_LEVELS |
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| 351 | TAUCUMV(K,NW,NG)=TAUCUMV(K-1,NW,NG)+DTAUKV(K,NW,NG) |
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| 352 | END DO |
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| 353 | END DO |
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| 354 | END DO ! end full gauss loop |
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| 355 | |
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| 356 | |
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| 357 | ! Titan's outputs (JVO, 2016)=============================================== |
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| 358 | ! do l=1,L_NLAYRAD |
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| 359 | ! do nw=1,L_NSPECTV |
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| 360 | ! INT_DTAU(L,NW) = 0.0d+0 |
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| 361 | ! DO NG=1,L_NGAUSS |
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| 362 | ! INT_DTAU(L,NW)= INT_DTAU(L,NW) + dtauv(L,nw,ng)*gweight(NG) |
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| 363 | ! enddo |
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| 364 | ! enddo |
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| 365 | ! enddo |
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| 366 | |
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| 367 | ! do nw=1,L_NSPECTV |
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| 368 | ! write(str2,'(i2.2)') nw |
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| 369 | ! call writediagfi(1,'kgv'//str2,'Gaz extinction coefficient VI band '//str2,'m-1',1,int_dtau(L_NLAYRAD:1:-1,nw)/dz_lay(L_NLAYRAD:1:-1)) |
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| 370 | ! call writediagfi(1,'khv'//str2,'Haze extinction coefficient VI band '//str2,'m-1',1,k_haze(L_NLAYRAD:1:-1,nw)/dz_lay(L_NLAYRAD:1:-1)) |
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| 371 | ! enddo |
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| 372 | |
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| 373 | ! ============================================================================== |
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| 374 | |
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| 375 | |
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| 376 | return |
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| 377 | |
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| 378 | |
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| 379 | end subroutine optcv |
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