Context Navigation

callcorrk.F90 @ 1956

Last change on this file since 1956 was 1947, checked in by jvatant, 7 years ago
Enables altitude-depending gravity field g(z) (glat->gzlat) in physics + Can be dangerous ( disagreement with dyn) but important (compulsive !) to have correct altitudes in the chemistry + Can be activated with eff_gz flag in callphys.def -- JVO
Property svn:executable set to ``*
File size: 19.3 KB

Rev	Line
[526]	1	subroutine callcorrk(ngrid,nlayer,pq,nq,qsurf, &
[1482]	2	albedo,albedo_equivalent,emis,mu0,pplev,pplay,pt, &
[1788]	3	tsurf,fract,dist_star, &
[253]	4	dtlw,dtsw,fluxsurf_lw, &
[1482]	5	fluxsurf_sw,fluxsurfabs_sw,fluxtop_lw, &
	6	fluxabs_sw,fluxtop_dn, &
[538]	7	OLR_nu,OSR_nu, &
[1822]	8	lastcall)
[253]	9
[1722]	10	use mod_phys_lmdz_para, only : is_master
[253]	11	use radinc_h
	12	use radcommon_h
[471]	13	use gases_h
[787]	14	USE tracer_h
[1822]	15	use callkeys_mod, only: global1d, szangle
[1384]	16	use comcstfi_mod, only: pi, mugaz, cpp
[1722]	17	use callkeys_mod, only: diurnal,tracer, &
[1647]	18	strictboundcorrk,specOLR
[787]	19
[253]	20	implicit none
	21
	22	!==================================================================
	23	!
	24	! Purpose
	25	! -------
	26	! Solve the radiative transfer using the correlated-k method for
	27	! the gaseous absorption and the Toon et al. (1989) method for
	28	! scatttering due to aerosols.
	29	!
	30	! Authors
	31	! -------
	32	! Emmanuel 01/2001, Forget 09/2001
	33	! Robin Wordsworth (2009)
	34	!
	35	!==================================================================
	36
	37	!-----------------------------------------------------------------------
	38	! Declaration of the arguments (INPUT - OUTPUT) on the LMD GCM grid
	39	! Layer #1 is the layer near the ground.
[1308]	40	! Layer #nlayer is the layer at the top.
[1483]	41	!-----------------------------------------------------------------------
[253]	42
[1483]	43
	44	! INPUT
	45	INTEGER,INTENT(IN) :: ngrid ! Number of atmospheric columns.
	46	INTEGER,INTENT(IN) :: nlayer ! Number of atmospheric layers.
[1897]	47	REAL,INTENT(IN) :: pq(ngrid,nlayer,nq) ! Tracers (X/m2).
[1483]	48	INTEGER,INTENT(IN) :: nq ! Number of tracers.
	49	REAL,INTENT(IN) :: qsurf(ngrid,nq) ! Tracers on surface (kg.m-2).
	50	REAL,INTENT(IN) :: albedo(ngrid,L_NSPECTV) ! Spectral Short Wavelengths Albedo. By MT2015
	51	REAL,INTENT(IN) :: emis(ngrid) ! Long Wave emissivity.
	52	REAL,INTENT(IN) :: mu0(ngrid) ! Cosine of sun incident angle.
	53	REAL,INTENT(IN) :: pplev(ngrid,nlayer+1) ! Inter-layer pressure (Pa).
	54	REAL,INTENT(IN) :: pplay(ngrid,nlayer) ! Mid-layer pressure (Pa).
	55	REAL,INTENT(IN) :: pt(ngrid,nlayer) ! Air temperature (K).
	56	REAL,INTENT(IN) :: tsurf(ngrid) ! Surface temperature (K).
	57	REAL,INTENT(IN) :: fract(ngrid) ! Fraction of day.
	58	REAL,INTENT(IN) :: dist_star ! Distance star-planet (AU).
	59	logical,intent(in) :: lastcall ! Signals last call to physics.
	60
	61	! OUTPUT
	62	REAL,INTENT(OUT) :: dtlw(ngrid,nlayer) ! Heating rate (K/s) due to LW radiation.
	63	REAL,INTENT(OUT) :: dtsw(ngrid,nlayer) ! Heating rate (K/s) due to SW radiation.
	64	REAL,INTENT(OUT) :: fluxsurf_lw(ngrid) ! Incident LW flux to surf (W/m2).
	65	REAL,INTENT(OUT) :: fluxsurf_sw(ngrid) ! Incident SW flux to surf (W/m2)
	66	REAL,INTENT(OUT) :: fluxsurfabs_sw(ngrid) ! Absorbed SW flux by the surface (W/m2). By MT2015.
	67	REAL,INTENT(OUT) :: fluxtop_lw(ngrid) ! Outgoing LW flux to space (W/m2).
	68	REAL,INTENT(OUT) :: fluxabs_sw(ngrid) ! SW flux absorbed by the planet (W/m2).
	69	REAL,INTENT(OUT) :: fluxtop_dn(ngrid) ! Incident top of atmosphere SW flux (W/m2).
	70	REAL,INTENT(OUT) :: OLR_nu(ngrid,L_NSPECTI) ! Outgoing LW radition in each band (Normalized to the band width (W/m2/cm-1).
	71	REAL,INTENT(OUT) :: OSR_nu(ngrid,L_NSPECTV) ! Outgoing SW radition in each band (Normalized to the band width (W/m2/cm-1).
[1722]	72	REAL,INTENT(OUT) :: albedo_equivalent(ngrid) ! Spectrally Integrated Albedo. For Diagnostic. By MT2015
[1483]	73
	74
[253]	75	!-----------------------------------------------------------------------
	76	! Declaration of the variables required by correlated-k subroutines
[1483]	77	! Numbered from top to bottom (unlike in the GCM)
	78	!-----------------------------------------------------------------------
[253]	79
	80	REAL*8 tmid(L_LEVELS),pmid(L_LEVELS)
	81	REAL*8 tlevrad(L_LEVELS),plevrad(L_LEVELS)
	82
[1483]	83	! Optical values for the optci/cv subroutines
[253]	84	REAL*8 stel(L_NSPECTV),stel_fract(L_NSPECTV)
	85	REAL*8 dtaui(L_NLAYRAD,L_NSPECTI,L_NGAUSS)
	86	REAL*8 dtauv(L_NLAYRAD,L_NSPECTV,L_NGAUSS)
	87	REAL*8 cosbv(L_NLAYRAD,L_NSPECTV,L_NGAUSS)
	88	REAL*8 cosbi(L_NLAYRAD,L_NSPECTI,L_NGAUSS)
	89	REAL*8 wbari(L_NLAYRAD,L_NSPECTI,L_NGAUSS)
	90	REAL*8 wbarv(L_NLAYRAD,L_NSPECTV,L_NGAUSS)
	91	REAL*8 tauv(L_NLEVRAD,L_NSPECTV,L_NGAUSS)
	92	REAL*8 taucumv(L_LEVELS,L_NSPECTV,L_NGAUSS)
	93	REAL*8 taucumi(L_LEVELS,L_NSPECTI,L_NGAUSS)
	94
[961]	95	REAL*8 nfluxtopv,nfluxtopi,nfluxtop,fluxtopvdn
[1483]	96	REAL*8 nfluxoutv_nu(L_NSPECTV) ! Outgoing band-resolved VI flux at TOA (W/m2).
	97	REAL*8 nfluxtopi_nu(L_NSPECTI) ! Net band-resolved IR flux at TOA (W/m2).
	98	REAL*8 fluxupi_nu(L_NLAYRAD,L_NSPECTI) ! For 1D diagnostic.
[253]	99	REAL*8 fmneti(L_NLAYRAD),fmnetv(L_NLAYRAD)
	100	REAL*8 fluxupv(L_NLAYRAD),fluxupi(L_NLAYRAD)
	101	REAL*8 fluxdnv(L_NLAYRAD),fluxdni(L_NLAYRAD)
[1482]	102	REAL*8 albi,acosz
[1483]	103	REAL*8 albv(L_NSPECTV) ! Spectral Visible Albedo.
[253]	104
[1788]	105	INTEGER ig,l,k,nw
[253]	106
	107	real*8 taugsurf(L_NSPECTV,L_NGAUSS-1)
	108	real*8 taugsurfi(L_NSPECTI,L_NGAUSS-1)
	109
	110	logical OLRz
	111	real*8 NFLUXGNDV_nu(L_NSPECTV)
[1648]	112
[1483]	113	! Included by MT for albedo calculations.
[1482]	114	REAL*8 albedo_temp(L_NSPECTV) ! For equivalent albedo calculation.
[1526]	115	REAL*8 surface_stellar_flux ! Stellar flux reaching the surface. Useful for equivalent albedo calculation.
[305]	116
[1483]	117
[253]	118	!=======================================================================
[1822]	119	! I. Initialization on every call
[1483]	120	!=======================================================================
	121
[1529]	122
[1483]	123	! How much light do we get ?
[253]	124	do nw=1,L_NSPECTV
	125	stel(nw)=stellarf(nw)/(dist_star**2)
	126	end do
	127
	128
[1483]	129	!-----------------------------------------------------------------------
	130	do ig=1,ngrid ! Starting Big Loop over every GCM column
[253]	131	!-----------------------------------------------------------------------
	132
[1483]	133
[253]	134	!=======================================================================
[1483]	135	! II. Transformation of the GCM variables
	136	!=======================================================================
[253]	137
[1483]	138
	139	! Albedo and Emissivity.
	140	albi=1-emis(ig) ! Long Wave.
	141	DO nw=1,L_NSPECTV ! Short Wave loop.
[1482]	142	albv(nw)=albedo(ig,nw)
[1529]	143	ENDDO
[253]	144
[1483]	145	if ((ngrid.eq.1).and.(global1d)) then ! Fixed zenith angle 'szangle' in 1D simulations w/ globally-averaged sunlight.
[253]	146	acosz = cos(pi*szangle/180.0)
	147	print*,'acosz=',acosz,', szangle=',szangle
	148	else
[1483]	149	acosz=mu0(ig) ! Cosine of sun incident angle : 3D simulations or local 1D simulations using latitude.
[253]	150	endif
	151
	152	!-----------------------------------------------------------------------
	153	! Pressure and temperature
[1483]	154	!-----------------------------------------------------------------------
[253]	155
	156	DO l=1,nlayer
	157	plevrad(2*l) = pplay(ig,nlayer+1-l)/scalep
	158	plevrad(2*l+1) = pplev(ig,nlayer+1-l)/scalep
	159	tlevrad(2*l) = pt(ig,nlayer+1-l)
	160	tlevrad(2*l+1) = (pt(ig,nlayer+1-l)+pt(ig,max(nlayer-l,1)))/2
	161	END DO
	162
[600]	163	plevrad(1) = 0.
[1483]	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.
[253]	165
	166	tlevrad(1) = tlevrad(2)
[1308]	167	tlevrad(2*nlayer+1)=tsurf(ig)
[253]	168
[1423]	169	pmid(1) = max(pgasmin,0.0001*plevrad(3))
	170	pmid(2) = pmid(1)
	171
[253]	172	tmid(1) = tlevrad(2)
[1423]	173	tmid(2) = tmid(1)
	174
	175	DO l=1,L_NLAYRAD-1
	176	tmid(2l+1) = tlevrad(2l+1)
	177	tmid(2l+2) = tlevrad(2l+1)
	178	pmid(2l+1) = plevrad(2l+1)
	179	pmid(2l+2) = plevrad(2l+1)
[253]	180	END DO
[1423]	181	pmid(L_LEVELS) = plevrad(L_LEVELS)
	182	tmid(L_LEVELS) = tlevrad(L_LEVELS)
[253]	183
[1423]	184	!!Alternative interpolation:
	185	! pmid(3) = pmid(1)
	186	! pmid(4) = pmid(1)
	187	! tmid(3) = tmid(1)
	188	! tmid(4) = tmid(1)
	189	! DO l=2,L_NLAYRAD-1
	190	! tmid(2l+1) = tlevrad(2l)
	191	! tmid(2l+2) = tlevrad(2l)
	192	! pmid(2l+1) = plevrad(2l)
	193	! pmid(2l+2) = plevrad(2l)
	194	! END DO
	195	! pmid(L_LEVELS) = plevrad(L_LEVELS-1)
	196	! tmid(L_LEVELS) = tlevrad(L_LEVELS-1)
	197
[1483]	198	! Test for out-of-bounds pressure.
[253]	199	if(plevrad(3).lt.pgasmin)then
	200	print*,'Minimum pressure is outside the radiative'
	201	print*,'transfer kmatrix bounds, exiting.'
	202	call abort
	203	elseif(plevrad(L_LEVELS).gt.pgasmax)then
	204	print*,'Maximum pressure is outside the radiative'
	205	print*,'transfer kmatrix bounds, exiting.'
	206	call abort
	207	endif
	208
[1483]	209	! Test for out-of-bounds temperature.
[253]	210	do k=1,L_LEVELS
	211	if(tlevrad(k).lt.tgasmin)then
	212	print*,'Minimum temperature is outside the radiative'
[1145]	213	print*,'transfer kmatrix bounds'
[858]	214	print*,"k=",k," tlevrad(k)=",tlevrad(k)
	215	print*,"tgasmin=",tgasmin
[1145]	216	if (strictboundcorrk) then
	217	call abort
	218	else
	219	print,'**********************************************'
	220	print*,'we allow model to continue with tlevrad=tgasmin'
	221	print*,' ... we assume we know what you are doing ... '
	222	print*,' ... but do not let this happen too often ... '
	223	print,'**********************************************'
[1147]	224	!tlevrad(k)=tgasmin
[1145]	225	endif
[253]	226	elseif(tlevrad(k).gt.tgasmax)then
[1648]	227	! print*,'Maximum temperature is outside the radiative'
	228	! print*,'transfer kmatrix bounds, exiting.'
	229	! print*,"k=",k," tlevrad(k)=",tlevrad(k)
	230	! print*,"tgasmax=",tgasmax
[1145]	231	if (strictboundcorrk) then
	232	call abort
	233	else
[1648]	234	! print,'**********************************************'
	235	! print*,'we allow model to continue with tlevrad=tgasmax'
	236	! print*,' ... we assume we know what you are doing ... '
	237	! print*,' ... but do not let this happen too often ... '
	238	! print,'**********************************************'
[1147]	239	!tlevrad(k)=tgasmax
[1145]	240	endif
[253]	241	endif
	242	enddo
[1016]	243	do k=1,L_NLAYRAD+1
	244	if(tmid(k).lt.tgasmin)then
	245	print*,'Minimum temperature is outside the radiative'
	246	print*,'transfer kmatrix bounds, exiting.'
[1145]	247	print*,"k=",k," tmid(k)=",tmid(k)
[1016]	248	print*,"tgasmin=",tgasmin
[1145]	249	if (strictboundcorrk) then
	250	call abort
	251	else
	252	print,'**********************************************'
	253	print*,'we allow model to continue with tmid=tgasmin'
	254	print*,' ... we assume we know what you are doing ... '
	255	print*,' ... but do not let this happen too often ... '
	256	print,'**********************************************'
	257	tmid(k)=tgasmin
	258	endif
[1016]	259	elseif(tmid(k).gt.tgasmax)then
[1648]	260	! print*,'Maximum temperature is outside the radiative'
	261	! print*,'transfer kmatrix bounds, exiting.'
	262	! print*,"k=",k," tmid(k)=",tmid(k)
	263	! print*,"tgasmax=",tgasmax
[1145]	264	if (strictboundcorrk) then
	265	call abort
	266	else
[1648]	267	! print,'**********************************************'
	268	! print*,'we allow model to continue with tmid=tgasmin'
	269	! print*,' ... we assume we know what you are doing ... '
	270	! print*,' ... but do not let this happen too often ... '
	271	! print,'**********************************************'
[1145]	272	tmid(k)=tgasmax
	273	endif
[1016]	274	endif
	275	enddo
[253]	276
	277	!=======================================================================
[1483]	278	! III. Calling the main radiative transfer subroutines
	279	!=======================================================================
[253]	280
[1947]	281	Cmk(:) = 0.01 * 1.0 / (gzlat(ig,:) * mugaz * 1.672621e-27) ! q_main=1.0 assumed.
	282	gzlat_ig(:) = gzlat(ig,:)
[253]	283
	284	!-----------------------------------------------------------------------
[1483]	285	! Short Wave Part
	286	!-----------------------------------------------------------------------
[253]	287
[1483]	288	if(fract(ig) .ge. 1.0e-4) then ! Only during daylight.
[787]	289	if((ngrid.eq.1).and.(global1d))then
[253]	290	do nw=1,L_NSPECTV
[1483]	291	stel_fract(nw)= stel(nw)* 0.25 / acosz ! globally averaged = divide by 4, and we correct for solar zenith angle
[253]	292	end do
	293	else
	294	do nw=1,L_NSPECTV
[1161]	295	stel_fract(nw)= stel(nw) * fract(ig)
[253]	296	end do
[1483]	297	endif
	298
[1897]	299	call optcv(pq(ig,:,1:nmicro),nlayer,plevrad,tmid,pmid, &
[1822]	300	dtauv,tauv,taucumv,wbarv,cosbv,tauray,taugsurf)
[253]	301
	302	call sfluxv(dtauv,tauv,taucumv,albv,dwnv,wbarv,cosbv, &
[1781]	303	acosz,stel_fract, &
	304	nfluxtopv,fluxtopvdn,nfluxoutv_nu,nfluxgndv_nu, &
[253]	305	fmnetv,fluxupv,fluxdnv,fzerov,taugsurf)
	306
[1483]	307	else ! During the night, fluxes = 0.
[962]	308	nfluxtopv = 0.0d0
[1529]	309	fluxtopvdn = 0.0d0
[962]	310	nfluxoutv_nu(:) = 0.0d0
	311	nfluxgndv_nu(:) = 0.0d0
[253]	312	do l=1,L_NLAYRAD
[962]	313	fmnetv(l)=0.0d0
	314	fluxupv(l)=0.0d0
	315	fluxdnv(l)=0.0d0
[253]	316	end do
	317	end if
	318
[1482]	319
[1526]	320	! Equivalent Albedo Calculation (for OUTPUT). MT2015
	321	if(fract(ig) .ge. 1.0e-4) then ! equivalent albedo makes sense only during daylight.
	322	surface_stellar_flux=sum(nfluxgndv_nu(1:L_NSPECTV))
	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.
[1529]	324	DO nw=1,L_NSPECTV
	325	albedo_temp(nw)=albedo(ig,nw)*nfluxgndv_nu(nw)
[1526]	326	ENDDO
[1529]	327	albedo_temp(1:L_NSPECTV)=albedo_temp(1:L_NSPECTV)/surface_stellar_flux
[1526]	328	albedo_equivalent(ig)=sum(albedo_temp(1:L_NSPECTV))
	329	else
	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.
	331	endif
[1529]	332	else
	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.
	334	endif
[1482]	335
	336
[253]	337	!-----------------------------------------------------------------------
[1483]	338	! Long Wave Part
	339	!-----------------------------------------------------------------------
[253]	340
[1897]	341	call optci(pq(ig,:,1:nmicro),nlayer,plevrad,tlevrad,tmid,pmid, &
[1822]	342	dtaui,taucumi,cosbi,wbari,taugsurfi)
[538]	343
[253]	344	call sfluxi(plevrad,tlevrad,dtaui,taucumi,ubari,albi, &
[1781]	345	wnoi,dwni,cosbi,wbari,nfluxtopi,nfluxtopi_nu, &
[253]	346	fmneti,fluxupi,fluxdni,fluxupi_nu,fzeroi,taugsurfi)
	347
	348	!-----------------------------------------------------------------------
	349	! Transformation of the correlated-k code outputs
	350	! (into dtlw, dtsw, fluxsurf_lw, fluxsurf_sw, fluxtop_lw, fluxtop_sw)
	351
	352	! Flux incident at the top of the atmosphere
[961]	353	fluxtop_dn(ig)=fluxtopvdn
[253]	354
	355	fluxtop_lw(ig) = real(nfluxtopi)
	356	fluxabs_sw(ig) = real(-nfluxtopv)
	357	fluxsurf_lw(ig) = real(fluxdni(L_NLAYRAD))
	358	fluxsurf_sw(ig) = real(fluxdnv(L_NLAYRAD))
[1482]	359
	360	! Flux absorbed by the surface. By MT2015.
	361	fluxsurfabs_sw(ig) = fluxsurf_sw(ig)*(1.-albedo_equivalent(ig))
[253]	362
	363	if(fluxtop_dn(ig).lt.0.0)then
	364	print*,'Achtung! fluxtop_dn has lost the plot!'
	365	print*,'fluxtop_dn=',fluxtop_dn(ig)
	366	print*,'acosz=',acosz
	367	print*,'temp= ',pt(ig,:)
	368	print*,'pplay= ',pplay(ig,:)
	369	call abort
	370	endif
	371
	372	! Spectral output, for exoplanet observational comparison
	373	if(specOLR)then
	374	do nw=1,L_NSPECTI
[526]	375	OLR_nu(ig,nw)=nfluxtopi_nu(nw)/DWNI(nw) !JL Normalize to the bandwidth
[253]	376	end do
	377	do nw=1,L_NSPECTV
[366]	378	!GSR_nu(ig,nw)=nfluxgndv_nu(nw)
[526]	379	OSR_nu(ig,nw)=nfluxoutv_nu(nw)/DWNV(nw) !JL Normalize to the bandwidth
[253]	380	end do
	381	endif
	382
	383	! Finally, the heating rates
	384
[586]	385	DO l=2,L_NLAYRAD
	386	dtsw(ig,L_NLAYRAD+1-l)=(fmnetv(l)-fmnetv(l-1)) &
[1947]	387	gzlat(ig,L_NLAYRAD+1-l)/(cppscalep(plevrad(2l+1)-plevrad(2*l-1)))
[586]	388	dtlw(ig,L_NLAYRAD+1-l)=(fmneti(l)-fmneti(l-1)) &
[1947]	389	gzlat(ig,L_NLAYRAD+1-l)/(cppscalep(plevrad(2l+1)-plevrad(2*l-1)))
[586]	390	END DO
[253]	391
	392	! These are values at top of atmosphere
[586]	393	dtsw(ig,L_NLAYRAD)=(fmnetv(1)-nfluxtopv) &
[1947]	394	gzlat(ig,L_NLAYRAD)/(cppscalep*(plevrad(3)-plevrad(1)))
[586]	395	dtlw(ig,L_NLAYRAD)=(fmneti(1)-nfluxtopi) &
[1947]	396	gzlat(ig,L_NLAYRAD)/(cppscalep*(plevrad(3)-plevrad(1)))
[253]	397
	398
[1483]	399	!-----------------------------------------------------------------------
	400	end do ! End of big loop over every GCM column.
	401	!-----------------------------------------------------------------------
[253]	402
[1483]	403
	404
[253]	405	!-----------------------------------------------------------------------
	406	! Additional diagnostics
[1483]	407	!-----------------------------------------------------------------------
[253]	408
[1483]	409	! IR spectral output, for exoplanet observational comparison
	410	if(lastcall.and.(ngrid.eq.1))then ! could disable the 1D output, they are in the diagfi and diagspec... JL12
[253]	411
[1483]	412	print*,'Saving scalar quantities in surf_vals.out...'
	413	print*,'psurf = ', pplev(1,1),' Pa'
	414	open(116,file='surf_vals.out')
	415	write(116,*) tsurf(1),pplev(1,1),fluxtop_dn(1), &
	416	real(-nfluxtopv),real(nfluxtopi)
	417	close(116)
[253]	418
[526]	419
[1483]	420	! USEFUL COMMENT - Do Not Remove.
	421	!
[526]	422	! if(specOLR)then
	423	! open(117,file='OLRnu.out')
	424	! do nw=1,L_NSPECTI
	425	! write(117,*) OLR_nu(1,nw)
	426	! enddo
	427	! close(117)
	428	!
	429	! open(127,file='OSRnu.out')
	430	! do nw=1,L_NSPECTV
	431	! write(127,*) OSR_nu(1,nw)
	432	! enddo
	433	! close(127)
	434	! endif
[253]	435
[1483]	436	! OLR vs altitude: do it as a .txt file.
	437	OLRz=.false.
	438	if(OLRz)then
	439	print*,'saving IR vertical flux for OLRz...'
	440	open(118,file='OLRz_plevs.out')
	441	open(119,file='OLRz.out')
	442	do l=1,L_NLAYRAD
	443	write(118,) plevrad(2l)
	444	do nw=1,L_NSPECTI
	445	write(119,*) fluxupi_nu(l,nw)
	446	enddo
	447	enddo
	448	close(118)
	449	close(119)
	450	endif
[253]	451
[305]	452	endif
[253]	453
[1483]	454	! See physiq.F for explanations about CLFvarying. This is temporary.
[1647]	455	if (lastcall) then
[470]	456	IF( ALLOCATED( gasi ) ) DEALLOCATE( gasi )
	457	IF( ALLOCATED( gasv ) ) DEALLOCATE( gasv )
[1315]	458	!$OMP BARRIER
	459	!$OMP MASTER
[470]	460	IF( ALLOCATED( pgasref ) ) DEALLOCATE( pgasref )
	461	IF( ALLOCATED( tgasref ) ) DEALLOCATE( tgasref )
	462	IF( ALLOCATED( pfgasref ) ) DEALLOCATE( pfgasref )
[1315]	463	!$OMP END MASTER
[1529]	464	!$OMP BARRIER
[470]	465	endif
	466
[716]	467
[253]	468	end subroutine callcorrk

Note: See TracBrowser for help on using the repository browser.

Download in other formats:

Original Format