| 1 | subroutine callcorrk(ngrid,nlayer,pq,nq,qsurf, & |
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| 2 | albedo,albedo_equivalent,emis,mu0,pplev,pplay,pt, & |
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| 3 | tsurf,fract,dist_star, & |
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| 4 | dtlw,dtsw,fluxsurf_lw, & |
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| 5 | fluxsurf_sw,fluxsurfabs_sw,fluxtop_lw, & |
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| 6 | fluxabs_sw,fluxtop_dn, & |
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| 7 | OLR_nu,OSR_nu, & |
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| 8 | lastcall) |
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| 9 | |
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| 10 | use mod_phys_lmdz_para, only : is_master |
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| 11 | use radinc_h |
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| 12 | use radcommon_h |
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| 13 | use gases_h |
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| 14 | USE tracer_h |
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| 15 | use callkeys_mod, only: global1d, szangle |
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| 16 | use comcstfi_mod, only: pi, mugaz, cpp |
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| 17 | use callkeys_mod, only: diurnal,tracer, & |
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| 18 | strictboundcorrk,specOLR |
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| 19 | |
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| 20 | implicit none |
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| 21 | |
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| 22 | !================================================================== |
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| 23 | ! |
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| 24 | ! Purpose |
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| 25 | ! ------- |
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| 26 | ! Solve the radiative transfer using the correlated-k method for |
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| 27 | ! the gaseous absorption and the Toon et al. (1989) method for |
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| 28 | ! scatttering due to aerosols. |
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| 29 | ! |
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| 30 | ! Authors |
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| 31 | ! ------- |
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| 32 | ! Emmanuel 01/2001, Forget 09/2001 |
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| 33 | ! Robin Wordsworth (2009) |
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| 34 | ! |
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| 35 | !================================================================== |
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| 36 | |
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| 37 | !----------------------------------------------------------------------- |
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| 38 | ! Declaration of the arguments (INPUT - OUTPUT) on the LMD GCM grid |
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| 39 | ! Layer #1 is the layer near the ground. |
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| 40 | ! Layer #nlayer is the layer at the top. |
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| 41 | !----------------------------------------------------------------------- |
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| 42 | |
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| 43 | |
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| 44 | ! INPUT |
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| 45 | INTEGER,INTENT(IN) :: ngrid ! Number of atmospheric columns. |
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| 46 | INTEGER,INTENT(IN) :: nlayer ! Number of atmospheric layers. |
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| 47 | REAL,INTENT(IN) :: pq(ngrid,nlayer,nq) ! Tracers (X/m2). |
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| 48 | INTEGER,INTENT(IN) :: nq ! Number of tracers. |
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| 49 | REAL,INTENT(IN) :: qsurf(ngrid,nq) ! Tracers on surface (kg.m-2). |
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| 50 | REAL,INTENT(IN) :: albedo(ngrid,L_NSPECTV) ! Spectral Short Wavelengths Albedo. By MT2015 |
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| 51 | REAL,INTENT(IN) :: emis(ngrid) ! Long Wave emissivity. |
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| 52 | REAL,INTENT(IN) :: mu0(ngrid) ! Cosine of sun incident angle. |
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| 53 | REAL,INTENT(IN) :: pplev(ngrid,nlayer+1) ! Inter-layer pressure (Pa). |
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| 54 | REAL,INTENT(IN) :: pplay(ngrid,nlayer) ! Mid-layer pressure (Pa). |
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| 55 | REAL,INTENT(IN) :: pt(ngrid,nlayer) ! Air temperature (K). |
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| 56 | REAL,INTENT(IN) :: tsurf(ngrid) ! Surface temperature (K). |
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| 57 | REAL,INTENT(IN) :: fract(ngrid) ! Fraction of day. |
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| 58 | REAL,INTENT(IN) :: dist_star ! Distance star-planet (AU). |
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| 59 | logical,intent(in) :: lastcall ! Signals last call to physics. |
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| 60 | |
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| 61 | ! OUTPUT |
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| 62 | REAL,INTENT(OUT) :: dtlw(ngrid,nlayer) ! Heating rate (K/s) due to LW radiation. |
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| 63 | REAL,INTENT(OUT) :: dtsw(ngrid,nlayer) ! Heating rate (K/s) due to SW radiation. |
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| 64 | REAL,INTENT(OUT) :: fluxsurf_lw(ngrid) ! Incident LW flux to surf (W/m2). |
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| 65 | REAL,INTENT(OUT) :: fluxsurf_sw(ngrid) ! Incident SW flux to surf (W/m2) |
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| 66 | REAL,INTENT(OUT) :: fluxsurfabs_sw(ngrid) ! Absorbed SW flux by the surface (W/m2). By MT2015. |
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| 67 | REAL,INTENT(OUT) :: fluxtop_lw(ngrid) ! Outgoing LW flux to space (W/m2). |
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| 68 | REAL,INTENT(OUT) :: fluxabs_sw(ngrid) ! SW flux absorbed by the planet (W/m2). |
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| 69 | REAL,INTENT(OUT) :: fluxtop_dn(ngrid) ! Incident top of atmosphere SW flux (W/m2). |
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| 70 | REAL,INTENT(OUT) :: OLR_nu(ngrid,L_NSPECTI) ! Outgoing LW radition in each band (Normalized to the band width (W/m2/cm-1). |
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| 71 | REAL,INTENT(OUT) :: OSR_nu(ngrid,L_NSPECTV) ! Outgoing SW radition in each band (Normalized to the band width (W/m2/cm-1). |
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| 72 | REAL,INTENT(OUT) :: albedo_equivalent(ngrid) ! Spectrally Integrated Albedo. For Diagnostic. By MT2015 |
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| 73 | |
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| 74 | |
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| 75 | !----------------------------------------------------------------------- |
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| 76 | ! Declaration of the variables required by correlated-k subroutines |
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| 77 | ! Numbered from top to bottom (unlike in the GCM) |
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| 78 | !----------------------------------------------------------------------- |
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| 79 | |
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| 80 | REAL*8 tmid(L_LEVELS),pmid(L_LEVELS) |
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| 81 | REAL*8 tlevrad(L_LEVELS),plevrad(L_LEVELS) |
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| 82 | |
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| 83 | ! Optical values for the optci/cv subroutines |
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| 84 | REAL*8 stel(L_NSPECTV),stel_fract(L_NSPECTV) |
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| 85 | REAL*8 dtaui(L_NLAYRAD,L_NSPECTI,L_NGAUSS) |
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| 86 | REAL*8 dtauv(L_NLAYRAD,L_NSPECTV,L_NGAUSS) |
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| 87 | REAL*8 cosbv(L_NLAYRAD,L_NSPECTV,L_NGAUSS) |
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| 88 | REAL*8 cosbi(L_NLAYRAD,L_NSPECTI,L_NGAUSS) |
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| 89 | REAL*8 wbari(L_NLAYRAD,L_NSPECTI,L_NGAUSS) |
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| 90 | REAL*8 wbarv(L_NLAYRAD,L_NSPECTV,L_NGAUSS) |
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| 91 | REAL*8 tauv(L_NLEVRAD,L_NSPECTV,L_NGAUSS) |
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| 92 | REAL*8 taucumv(L_LEVELS,L_NSPECTV,L_NGAUSS) |
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| 93 | REAL*8 taucumi(L_LEVELS,L_NSPECTI,L_NGAUSS) |
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| 94 | |
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| 95 | REAL*8 nfluxtopv,nfluxtopi,nfluxtop,fluxtopvdn |
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| 96 | REAL*8 nfluxoutv_nu(L_NSPECTV) ! Outgoing band-resolved VI flux at TOA (W/m2). |
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| 97 | REAL*8 nfluxtopi_nu(L_NSPECTI) ! Net band-resolved IR flux at TOA (W/m2). |
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| 98 | REAL*8 fluxupi_nu(L_NLAYRAD,L_NSPECTI) ! For 1D diagnostic. |
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| 99 | REAL*8 fmneti(L_NLAYRAD),fmnetv(L_NLAYRAD) |
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| 100 | REAL*8 fluxupv(L_NLAYRAD),fluxupi(L_NLAYRAD) |
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| 101 | REAL*8 fluxdnv(L_NLAYRAD),fluxdni(L_NLAYRAD) |
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| 102 | REAL*8 albi,acosz |
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| 103 | REAL*8 albv(L_NSPECTV) ! Spectral Visible Albedo. |
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| 104 | |
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| 105 | INTEGER ig,l,k,nw |
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| 106 | |
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| 107 | real*8 taugsurf(L_NSPECTV,L_NGAUSS-1) |
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| 108 | real*8 taugsurfi(L_NSPECTI,L_NGAUSS-1) |
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| 109 | |
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| 110 | logical OLRz |
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| 111 | real*8 NFLUXGNDV_nu(L_NSPECTV) |
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| 112 | |
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| 113 | ! Included by MT for albedo calculations. |
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| 114 | REAL*8 albedo_temp(L_NSPECTV) ! For equivalent albedo calculation. |
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| 115 | REAL*8 surface_stellar_flux ! Stellar flux reaching the surface. Useful for equivalent albedo calculation. |
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| 116 | |
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| 117 | |
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| 118 | !======================================================================= |
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| 119 | ! I. Initialization on every call |
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| 120 | !======================================================================= |
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| 121 | |
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| 122 | |
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| 123 | ! How much light do we get ? |
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| 124 | do nw=1,L_NSPECTV |
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| 125 | stel(nw)=stellarf(nw)/(dist_star**2) |
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| 126 | end do |
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| 127 | |
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| 128 | |
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| 129 | !----------------------------------------------------------------------- |
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| 130 | do ig=1,ngrid ! Starting Big Loop over every GCM column |
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| 131 | !----------------------------------------------------------------------- |
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| 132 | |
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| 133 | |
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| 134 | !======================================================================= |
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| 135 | ! II. Transformation of the GCM variables |
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| 136 | !======================================================================= |
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| 137 | |
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| 138 | |
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| 139 | ! Albedo and Emissivity. |
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| 140 | albi=1-emis(ig) ! Long Wave. |
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| 141 | DO nw=1,L_NSPECTV ! Short Wave loop. |
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| 142 | albv(nw)=albedo(ig,nw) |
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| 143 | ENDDO |
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| 144 | |
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| 145 | if ((ngrid.eq.1).and.(global1d)) then ! Fixed zenith angle 'szangle' in 1D simulations w/ globally-averaged sunlight. |
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| 146 | acosz = cos(pi*szangle/180.0) |
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| 147 | print*,'acosz=',acosz,', szangle=',szangle |
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| 148 | else |
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| 149 | acosz=mu0(ig) ! Cosine of sun incident angle : 3D simulations or local 1D simulations using latitude. |
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| 150 | endif |
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| 151 | |
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| 152 | !----------------------------------------------------------------------- |
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| 153 | ! Pressure and temperature |
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| 154 | !----------------------------------------------------------------------- |
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| 155 | |
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| 156 | DO l=1,nlayer |
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| 157 | plevrad(2*l) = pplay(ig,nlayer+1-l)/scalep |
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| 158 | plevrad(2*l+1) = pplev(ig,nlayer+1-l)/scalep |
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| 159 | tlevrad(2*l) = pt(ig,nlayer+1-l) |
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| 160 | tlevrad(2*l+1) = (pt(ig,nlayer+1-l)+pt(ig,max(nlayer-l,1)))/2 |
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| 161 | END DO |
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| 162 | |
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| 163 | plevrad(1) = 0. |
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| 164 | plevrad(2) = 0. !! Trick to have correct calculations of fluxes in gflux(i/v).F, but the pmid levels are not impacted by this change. |
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| 165 | |
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| 166 | tlevrad(1) = tlevrad(2) |
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| 167 | tlevrad(2*nlayer+1)=tsurf(ig) |
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| 168 | |
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| 169 | pmid(1) = max(pgasmin,0.0001*plevrad(3)) |
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| 170 | pmid(2) = pmid(1) |
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| 171 | |
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| 172 | tmid(1) = tlevrad(2) |
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| 173 | tmid(2) = tmid(1) |
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| 174 | |
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| 175 | DO l=1,L_NLAYRAD-1 |
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| 176 | tmid(2*l+1) = tlevrad(2*l+1) |
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| 177 | tmid(2*l+2) = tlevrad(2*l+1) |
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| 178 | pmid(2*l+1) = plevrad(2*l+1) |
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| 179 | pmid(2*l+2) = plevrad(2*l+1) |
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| 180 | END DO |
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| 181 | pmid(L_LEVELS) = plevrad(L_LEVELS) |
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| 182 | tmid(L_LEVELS) = tlevrad(L_LEVELS) |
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| 183 | |
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| 184 | !!Alternative interpolation: |
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| 185 | ! pmid(3) = pmid(1) |
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| 186 | ! pmid(4) = pmid(1) |
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| 187 | ! tmid(3) = tmid(1) |
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| 188 | ! tmid(4) = tmid(1) |
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| 189 | ! DO l=2,L_NLAYRAD-1 |
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| 190 | ! tmid(2*l+1) = tlevrad(2*l) |
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| 191 | ! tmid(2*l+2) = tlevrad(2*l) |
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| 192 | ! pmid(2*l+1) = plevrad(2*l) |
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| 193 | ! pmid(2*l+2) = plevrad(2*l) |
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| 194 | ! END DO |
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| 195 | ! pmid(L_LEVELS) = plevrad(L_LEVELS-1) |
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| 196 | ! tmid(L_LEVELS) = tlevrad(L_LEVELS-1) |
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| 197 | |
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| 198 | ! Test for out-of-bounds pressure. |
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| 199 | if(plevrad(3).lt.pgasmin)then |
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| 200 | print*,'Minimum pressure is outside the radiative' |
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| 201 | print*,'transfer kmatrix bounds, exiting.' |
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| 202 | call abort |
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| 203 | elseif(plevrad(L_LEVELS).gt.pgasmax)then |
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| 204 | print*,'Maximum pressure is outside the radiative' |
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| 205 | print*,'transfer kmatrix bounds, exiting.' |
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| 206 | call abort |
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| 207 | endif |
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| 208 | |
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| 209 | ! Test for out-of-bounds temperature. |
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| 210 | do k=1,L_LEVELS |
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| 211 | if(tlevrad(k).lt.tgasmin)then |
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| 212 | print*,'Minimum temperature is outside the radiative' |
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| 213 | print*,'transfer kmatrix bounds' |
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| 214 | print*,"k=",k," tlevrad(k)=",tlevrad(k) |
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| 215 | print*,"tgasmin=",tgasmin |
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| 216 | if (strictboundcorrk) then |
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| 217 | call abort |
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| 218 | else |
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| 219 | print*,'***********************************************' |
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| 220 | print*,'we allow model to continue with tlevrad=tgasmin' |
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| 221 | print*,' ... we assume we know what you are doing ... ' |
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| 222 | print*,' ... but do not let this happen too often ... ' |
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| 223 | print*,'***********************************************' |
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| 224 | !tlevrad(k)=tgasmin |
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| 225 | endif |
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| 226 | elseif(tlevrad(k).gt.tgasmax)then |
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| 227 | ! print*,'Maximum temperature is outside the radiative' |
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| 228 | ! print*,'transfer kmatrix bounds, exiting.' |
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| 229 | ! print*,"k=",k," tlevrad(k)=",tlevrad(k) |
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| 230 | ! print*,"tgasmax=",tgasmax |
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| 231 | if (strictboundcorrk) then |
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| 232 | call abort |
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| 233 | else |
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| 234 | ! print*,'***********************************************' |
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| 235 | ! print*,'we allow model to continue with tlevrad=tgasmax' |
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| 236 | ! print*,' ... we assume we know what you are doing ... ' |
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| 237 | ! print*,' ... but do not let this happen too often ... ' |
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| 238 | ! print*,'***********************************************' |
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| 239 | !tlevrad(k)=tgasmax |
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| 240 | endif |
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| 241 | endif |
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| 242 | enddo |
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| 243 | do k=1,L_NLAYRAD+1 |
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| 244 | if(tmid(k).lt.tgasmin)then |
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| 245 | print*,'Minimum temperature is outside the radiative' |
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| 246 | print*,'transfer kmatrix bounds, exiting.' |
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| 247 | print*,"k=",k," tmid(k)=",tmid(k) |
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| 248 | print*,"tgasmin=",tgasmin |
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| 249 | if (strictboundcorrk) then |
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| 250 | call abort |
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| 251 | else |
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| 252 | print*,'***********************************************' |
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| 253 | print*,'we allow model to continue with tmid=tgasmin' |
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| 254 | print*,' ... we assume we know what you are doing ... ' |
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| 255 | print*,' ... but do not let this happen too often ... ' |
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| 256 | print*,'***********************************************' |
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| 257 | tmid(k)=tgasmin |
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| 258 | endif |
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| 259 | elseif(tmid(k).gt.tgasmax)then |
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| 260 | ! print*,'Maximum temperature is outside the radiative' |
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| 261 | ! print*,'transfer kmatrix bounds, exiting.' |
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| 262 | ! print*,"k=",k," tmid(k)=",tmid(k) |
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| 263 | ! print*,"tgasmax=",tgasmax |
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| 264 | if (strictboundcorrk) then |
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| 265 | call abort |
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| 266 | else |
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| 267 | ! print*,'***********************************************' |
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| 268 | ! print*,'we allow model to continue with tmid=tgasmin' |
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| 269 | ! print*,' ... we assume we know what you are doing ... ' |
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| 270 | ! print*,' ... but do not let this happen too often ... ' |
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| 271 | ! print*,'***********************************************' |
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| 272 | tmid(k)=tgasmax |
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| 273 | endif |
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| 274 | endif |
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| 275 | enddo |
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| 276 | |
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| 277 | !======================================================================= |
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| 278 | ! III. Calling the main radiative transfer subroutines |
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| 279 | !======================================================================= |
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| 280 | |
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| 281 | Cmk(:) = 0.01 * 1.0 / (gzlat(ig,:) * mugaz * 1.672621e-27) ! q_main=1.0 assumed. |
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| 282 | gzlat_ig(:) = gzlat(ig,:) |
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| 283 | |
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| 284 | !----------------------------------------------------------------------- |
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| 285 | ! Short Wave Part |
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| 286 | !----------------------------------------------------------------------- |
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| 287 | |
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| 288 | if(fract(ig) .ge. 1.0e-4) then ! Only during daylight. |
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| 289 | if((ngrid.eq.1).and.(global1d))then |
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| 290 | do nw=1,L_NSPECTV |
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| 291 | stel_fract(nw)= stel(nw)* 0.25 / acosz ! globally averaged = divide by 4, and we correct for solar zenith angle |
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| 292 | end do |
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| 293 | else |
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| 294 | do nw=1,L_NSPECTV |
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| 295 | stel_fract(nw)= stel(nw) * fract(ig) |
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| 296 | end do |
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| 297 | endif |
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| 298 | |
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| 299 | call optcv(pq(ig,:,1:nmicro),nlayer,plevrad,tmid,pmid, & |
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| 300 | dtauv,tauv,taucumv,wbarv,cosbv,tauray,taugsurf) |
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| 301 | |
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| 302 | call sfluxv(dtauv,tauv,taucumv,albv,dwnv,wbarv,cosbv, & |
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| 303 | acosz,stel_fract, & |
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| 304 | nfluxtopv,fluxtopvdn,nfluxoutv_nu,nfluxgndv_nu, & |
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| 305 | fmnetv,fluxupv,fluxdnv,fzerov,taugsurf) |
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| 306 | |
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| 307 | else ! During the night, fluxes = 0. |
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| 308 | nfluxtopv = 0.0d0 |
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| 309 | fluxtopvdn = 0.0d0 |
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| 310 | nfluxoutv_nu(:) = 0.0d0 |
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| 311 | nfluxgndv_nu(:) = 0.0d0 |
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| 312 | do l=1,L_NLAYRAD |
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| 313 | fmnetv(l)=0.0d0 |
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| 314 | fluxupv(l)=0.0d0 |
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| 315 | fluxdnv(l)=0.0d0 |
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| 316 | end do |
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| 317 | end if |
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| 318 | |
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| 319 | |
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| 320 | ! Equivalent Albedo Calculation (for OUTPUT). MT2015 |
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| 321 | if(fract(ig) .ge. 1.0e-4) then ! equivalent albedo makes sense only during daylight. |
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| 322 | surface_stellar_flux=sum(nfluxgndv_nu(1:L_NSPECTV)) |
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| 323 | if(surface_stellar_flux .gt. 1.0e-3) then ! equivalent albedo makes sense only if the stellar flux received by the surface is positive. |
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| 324 | DO nw=1,L_NSPECTV |
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| 325 | albedo_temp(nw)=albedo(ig,nw)*nfluxgndv_nu(nw) |
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| 326 | ENDDO |
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| 327 | albedo_temp(1:L_NSPECTV)=albedo_temp(1:L_NSPECTV)/surface_stellar_flux |
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| 328 | albedo_equivalent(ig)=sum(albedo_temp(1:L_NSPECTV)) |
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| 329 | else |
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| 330 | albedo_equivalent(ig)=0.0 ! Spectrally Integrated Albedo not defined for non-irradiated grid points. So we arbitrary set the equivalent albedo to 0. |
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| 331 | endif |
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| 332 | else |
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| 333 | albedo_equivalent(ig)=0.0 ! Spectrally Integrated Albedo not defined for non-irradiated grid points. So we arbitrary set the equivalent albedo to 0. |
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| 334 | endif |
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| 335 | |
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| 336 | |
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| 337 | !----------------------------------------------------------------------- |
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| 338 | ! Long Wave Part |
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| 339 | !----------------------------------------------------------------------- |
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| 340 | |
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| 341 | call optci(pq(ig,:,1:nmicro),nlayer,plevrad,tlevrad,tmid,pmid, & |
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| 342 | dtaui,taucumi,cosbi,wbari,taugsurfi) |
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| 343 | |
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| 344 | call sfluxi(plevrad,tlevrad,dtaui,taucumi,ubari,albi, & |
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| 345 | wnoi,dwni,cosbi,wbari,nfluxtopi,nfluxtopi_nu, & |
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| 346 | fmneti,fluxupi,fluxdni,fluxupi_nu,fzeroi,taugsurfi) |
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| 347 | |
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| 348 | !----------------------------------------------------------------------- |
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| 349 | ! Transformation of the correlated-k code outputs |
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| 350 | ! (into dtlw, dtsw, fluxsurf_lw, fluxsurf_sw, fluxtop_lw, fluxtop_sw) |
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| 351 | |
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| 352 | ! Flux incident at the top of the atmosphere |
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| 353 | fluxtop_dn(ig)=fluxtopvdn |
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| 354 | |
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| 355 | fluxtop_lw(ig) = real(nfluxtopi) |
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| 356 | fluxabs_sw(ig) = real(-nfluxtopv) |
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| 357 | fluxsurf_lw(ig) = real(fluxdni(L_NLAYRAD)) |
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| 358 | fluxsurf_sw(ig) = real(fluxdnv(L_NLAYRAD)) |
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| 359 | |
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| 360 | ! Flux absorbed by the surface. By MT2015. |
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| 361 | fluxsurfabs_sw(ig) = fluxsurf_sw(ig)*(1.-albedo_equivalent(ig)) |
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| 362 | |
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| 363 | if(fluxtop_dn(ig).lt.0.0)then |
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| 364 | print*,'Achtung! fluxtop_dn has lost the plot!' |
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| 365 | print*,'fluxtop_dn=',fluxtop_dn(ig) |
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| 366 | print*,'acosz=',acosz |
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| 367 | print*,'temp= ',pt(ig,:) |
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| 368 | print*,'pplay= ',pplay(ig,:) |
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| 369 | call abort |
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| 370 | endif |
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| 371 | |
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| 372 | ! Spectral output, for exoplanet observational comparison |
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| 373 | if(specOLR)then |
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| 374 | do nw=1,L_NSPECTI |
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| 375 | OLR_nu(ig,nw)=nfluxtopi_nu(nw)/DWNI(nw) !JL Normalize to the bandwidth |
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| 376 | end do |
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| 377 | do nw=1,L_NSPECTV |
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| 378 | !GSR_nu(ig,nw)=nfluxgndv_nu(nw) |
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| 379 | OSR_nu(ig,nw)=nfluxoutv_nu(nw)/DWNV(nw) !JL Normalize to the bandwidth |
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| 380 | end do |
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| 381 | endif |
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| 382 | |
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| 383 | ! Finally, the heating rates |
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| 384 | |
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| 385 | DO l=2,L_NLAYRAD |
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| 386 | dtsw(ig,L_NLAYRAD+1-l)=(fmnetv(l)-fmnetv(l-1)) & |
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| 387 | *gzlat(ig,L_NLAYRAD+1-l)/(cpp*scalep*(plevrad(2*l+1)-plevrad(2*l-1))) |
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| 388 | dtlw(ig,L_NLAYRAD+1-l)=(fmneti(l)-fmneti(l-1)) & |
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| 389 | *gzlat(ig,L_NLAYRAD+1-l)/(cpp*scalep*(plevrad(2*l+1)-plevrad(2*l-1))) |
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| 390 | END DO |
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| 391 | |
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| 392 | ! These are values at top of atmosphere |
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| 393 | dtsw(ig,L_NLAYRAD)=(fmnetv(1)-nfluxtopv) & |
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| 394 | *gzlat(ig,L_NLAYRAD)/(cpp*scalep*(plevrad(3)-plevrad(1))) |
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| 395 | dtlw(ig,L_NLAYRAD)=(fmneti(1)-nfluxtopi) & |
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| 396 | *gzlat(ig,L_NLAYRAD)/(cpp*scalep*(plevrad(3)-plevrad(1))) |
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| 397 | |
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| 398 | |
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| 399 | !----------------------------------------------------------------------- |
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| 400 | end do ! End of big loop over every GCM column. |
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| 401 | !----------------------------------------------------------------------- |
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| 402 | |
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| 403 | |
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| 404 | |
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| 405 | !----------------------------------------------------------------------- |
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| 406 | ! Additional diagnostics |
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| 407 | !----------------------------------------------------------------------- |
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| 408 | |
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| 409 | ! IR spectral output, for exoplanet observational comparison |
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| 410 | if(lastcall.and.(ngrid.eq.1))then ! could disable the 1D output, they are in the diagfi and diagspec... JL12 |
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| 411 | |
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| 412 | print*,'Saving scalar quantities in surf_vals.out...' |
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| 413 | print*,'psurf = ', pplev(1,1),' Pa' |
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| 414 | open(116,file='surf_vals.out') |
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| 415 | write(116,*) tsurf(1),pplev(1,1),fluxtop_dn(1), & |
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| 416 | real(-nfluxtopv),real(nfluxtopi) |
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| 417 | close(116) |
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| 418 | |
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| 419 | |
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| 420 | ! USEFUL COMMENT - Do Not Remove. |
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| 421 | ! |
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| 422 | ! if(specOLR)then |
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| 423 | ! open(117,file='OLRnu.out') |
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| 424 | ! do nw=1,L_NSPECTI |
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| 425 | ! write(117,*) OLR_nu(1,nw) |
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| 426 | ! enddo |
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| 427 | ! close(117) |
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| 428 | ! |
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| 429 | ! open(127,file='OSRnu.out') |
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| 430 | ! do nw=1,L_NSPECTV |
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| 431 | ! write(127,*) OSR_nu(1,nw) |
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| 432 | ! enddo |
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| 433 | ! close(127) |
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| 434 | ! endif |
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| 435 | |
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| 436 | ! OLR vs altitude: do it as a .txt file. |
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| 437 | OLRz=.false. |
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| 438 | if(OLRz)then |
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| 439 | print*,'saving IR vertical flux for OLRz...' |
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| 440 | open(118,file='OLRz_plevs.out') |
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| 441 | open(119,file='OLRz.out') |
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| 442 | do l=1,L_NLAYRAD |
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| 443 | write(118,*) plevrad(2*l) |
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| 444 | do nw=1,L_NSPECTI |
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| 445 | write(119,*) fluxupi_nu(l,nw) |
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| 446 | enddo |
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| 447 | enddo |
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| 448 | close(118) |
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| 449 | close(119) |
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| 450 | endif |
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| 451 | |
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| 452 | endif |
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| 453 | |
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| 454 | ! See physiq.F for explanations about CLFvarying. This is temporary. |
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| 455 | if (lastcall) then |
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| 456 | IF( ALLOCATED( gasi ) ) DEALLOCATE( gasi ) |
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| 457 | IF( ALLOCATED( gasv ) ) DEALLOCATE( gasv ) |
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| 458 | !$OMP BARRIER |
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| 459 | !$OMP MASTER |
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| 460 | IF( ALLOCATED( pgasref ) ) DEALLOCATE( pgasref ) |
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| 461 | IF( ALLOCATED( tgasref ) ) DEALLOCATE( tgasref ) |
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| 462 | IF( ALLOCATED( pfgasref ) ) DEALLOCATE( pfgasref ) |
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| 463 | !$OMP END MASTER |
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| 464 | !$OMP BARRIER |
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| 465 | endif |
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| 466 | |
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| 467 | |
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| 468 | end subroutine callcorrk |
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