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callcorrk.F90 @ 3026

Last change on this file since 3026 was 2408, checked in by jvatant, 4 years ago
Titan GCM : Fix a bug in corrk-recombining scheme optimisation. --JVO
Property svn:executable set to ``*
File size: 27.6 KB

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1	subroutine callcorrk(ngrid,nlayer,pq,nq,qsurf,zday, &
2	albedo,albedo_equivalent,emis,mu0,pplev,pplay,pt, &
3	tsurf,fract,dist_star, &
4	dtlw,dtsw,fluxsurf_lw, &
5	fluxsurf_sw,fluxsurfabs_sw,fluxtop_lw, &
6	fluxabs_sw,fluxtop_dn, &
7	OLR_nu,OSR_nu, &
8	int_dtaui,int_dtauv, &
9	lastcall)
10
11	use mod_phys_lmdz_para, only : is_master
12	use radinc_h
13	use radcommon_h
14	use gases_h
15	USE tracer_h
16	use callkeys_mod, only: global1d, szangle
17	use comcstfi_mod, only: pi, mugaz, cpp
18	use callkeys_mod, only: diurnal,tracer,seashaze,corrk_recombin, &
19	strictboundcorrk,specOLR,diagdtau, &
20	tplanckmin,tplanckmax
21	use geometry_mod, only: latitude
22
23	implicit none
24
25	!==================================================================
26	!
27	! Purpose
28	! -------
29	! Solve the radiative transfer using the correlated-k method for
30	! the gaseous absorption and the Toon et al. (1989) method for
31	! scatttering due to aerosols.
32	!
33	! Authors
34	! -------
35	! Emmanuel 01/2001, Forget 09/2001
36	! Robin Wordsworth (2009)
37	! Jan Vatant d'Ollone (2018) -> corrk recombining case
38	!
39	!==================================================================
40
41	!-----------------------------------------------------------------------
42	! Declaration of the arguments (INPUT - OUTPUT) on the LMD GCM grid
43	! Layer #1 is the layer near the ground.
44	! Layer #nlayer is the layer at the top.
45	!-----------------------------------------------------------------------
46
47
48	! INPUT
49	INTEGER,INTENT(IN) :: ngrid ! Number of atmospheric columns.
50	INTEGER,INTENT(IN) :: nlayer ! Number of atmospheric layers.
51	REAL,INTENT(IN) :: pq(ngrid,nlayer,nq) ! Tracers (X/kg).
52	INTEGER,INTENT(IN) :: nq ! Number of tracers.
53	REAL,INTENT(IN) :: qsurf(ngrid,nq) ! Tracers on surface (kg.m-2).
54	REAL,INTENT(IN) :: zday ! Time elapsed since Ls=0 (sols).
55	REAL,INTENT(IN) :: albedo(ngrid,L_NSPECTV) ! Spectral Short Wavelengths Albedo. By MT2015
56	REAL,INTENT(IN) :: emis(ngrid) ! Long Wave emissivity.
57	REAL,INTENT(IN) :: mu0(ngrid) ! Cosine of sun incident angle.
58	REAL,INTENT(IN) :: pplev(ngrid,nlayer+1) ! Inter-layer pressure (Pa).
59	REAL,INTENT(IN) :: pplay(ngrid,nlayer) ! Mid-layer pressure (Pa).
60	REAL,INTENT(IN) :: pt(ngrid,nlayer) ! Air temperature (K).
61	REAL,INTENT(IN) :: tsurf(ngrid) ! Surface temperature (K).
62	REAL,INTENT(IN) :: fract(ngrid) ! Fraction of day.
63	REAL,INTENT(IN) :: dist_star ! Distance star-planet (AU).
64	logical,intent(in) :: lastcall ! Signals last call to physics.
65
66	! OUTPUT
67	REAL,INTENT(OUT) :: dtlw(ngrid,nlayer) ! Heating rate (K/s) due to LW radiation.
68	REAL,INTENT(OUT) :: dtsw(ngrid,nlayer) ! Heating rate (K/s) due to SW radiation.
69	REAL,INTENT(OUT) :: fluxsurf_lw(ngrid) ! Incident LW flux to surf (W/m2).
70	REAL,INTENT(OUT) :: fluxsurf_sw(ngrid) ! Incident SW flux to surf (W/m2)
71	REAL,INTENT(OUT) :: fluxsurfabs_sw(ngrid) ! Absorbed SW flux by the surface (W/m2). By MT2015.
72	REAL,INTENT(OUT) :: fluxtop_lw(ngrid) ! Outgoing LW flux to space (W/m2).
73	REAL,INTENT(OUT) :: fluxabs_sw(ngrid) ! SW flux absorbed by the planet (W/m2).
74	REAL,INTENT(OUT) :: fluxtop_dn(ngrid) ! Incident top of atmosphere SW flux (W/m2).
75	REAL,INTENT(OUT) :: OLR_nu(ngrid,L_NSPECTI) ! Outgoing LW radition in each band (Normalized to the band width (W/m2/cm-1).
76	REAL,INTENT(OUT) :: OSR_nu(ngrid,L_NSPECTV) ! Outgoing SW radition in each band (Normalized to the band width (W/m2/cm-1).
77	REAL,INTENT(OUT) :: albedo_equivalent(ngrid) ! Spectrally Integrated Albedo. For Diagnostic. By MT2015
78	REAL,INTENT(OUT) :: int_dtaui(ngrid,nlayer,L_NSPECTI) ! VI optical thickness of layers within narrowbands for diags ().
79	REAL,INTENT(OUT) :: int_dtauv(ngrid,nlayer,L_NSPECTV) ! IR optical thickness of layers within narrowbands for diags ().
80
81
82	!-----------------------------------------------------------------------
83	! Declaration of the variables required by correlated-k subroutines
84	! Numbered from top to bottom (unlike in the GCM)
85	!-----------------------------------------------------------------------
86
87	REAL*8 tmid(L_LEVELS),pmid(L_LEVELS)
88	REAL*8 tlevrad(L_LEVELS),plevrad(L_LEVELS)
89
90	! Optical values for the optci/cv subroutines
91	REAL*8 stel(L_NSPECTV),stel_fract(L_NSPECTV)
92	REAL*8 dtaui(L_NLAYRAD,L_NSPECTI,L_NGAUSS)
93	REAL*8 dtauv(L_NLAYRAD,L_NSPECTV,L_NGAUSS)
94	REAL*8 cosbv(L_NLAYRAD,L_NSPECTV,L_NGAUSS)
95	REAL*8 cosbi(L_NLAYRAD,L_NSPECTI,L_NGAUSS)
96	REAL*8 wbari(L_NLAYRAD,L_NSPECTI,L_NGAUSS)
97	REAL*8 wbarv(L_NLAYRAD,L_NSPECTV,L_NGAUSS)
98	REAL*8 tauv(L_NLEVRAD,L_NSPECTV,L_NGAUSS)
99	REAL*8 taucumv(L_LEVELS,L_NSPECTV,L_NGAUSS)
100	REAL*8 taucumi(L_LEVELS,L_NSPECTI,L_NGAUSS)
101
102	REAL*8 nfluxtopv,nfluxtopi,nfluxtop,fluxtopvdn
103	REAL*8 nfluxoutv_nu(L_NSPECTV) ! Outgoing band-resolved VI flux at TOA (W/m2).
104	REAL*8 nfluxtopi_nu(L_NSPECTI) ! Net band-resolved IR flux at TOA (W/m2).
105	REAL*8 fluxupi_nu(L_NLAYRAD,L_NSPECTI) ! For 1D diagnostic.
106	REAL*8 fmneti(L_NLAYRAD),fmnetv(L_NLAYRAD)
107	REAL*8 fluxupv(L_NLAYRAD),fluxupi(L_NLAYRAD)
108	REAL*8 fluxdnv(L_NLAYRAD),fluxdni(L_NLAYRAD)
109	REAL*8 albi,acosz
110	REAL*8 albv(L_NSPECTV) ! Spectral Visible Albedo.
111
112	INTEGER ig,l,k,nw,iq,ip,ilay,it
113
114	LOGICAL found
115
116	real*8 taugsurf(L_NSPECTV,L_NGAUSS-1)
117	real*8 taugsurfi(L_NSPECTI,L_NGAUSS-1)
118
119	! Miscellaneous :
120	character(len=100) :: message
121	character(len=10),parameter :: subname="callcorrk"
122
123	logical OLRz
124	real*8 NFLUXGNDV_nu(L_NSPECTV)
125
126	! Included by MT for albedo calculations.
127	REAL*8 albedo_temp(L_NSPECTV) ! For equivalent albedo calculation.
128	REAL*8 surface_stellar_flux ! Stellar flux reaching the surface. Useful for equivalent albedo calculation.
129
130	! For variable haze
131	REAL*8 seashazefact(L_LEVELS)
132
133	! For muphys optics
134	REAL*8 pqmo(ngrid,nlayer,nmicro) ! Tracers for microphysics optics (X/m2).
135	REAL*8 i2e(ngrid,nlayer) ! int 2 ext factor ( X.kg-1 -> X.m-2 for optics )
136
137	! For corr-k recombining
138	REAL*8 pqr(ngrid,L_PINT,L_REFVAR) ! Tracers for corr-k recombining (mol/mol).
139	REAL*8 fact, tmin, tmax
140
141	LOGICAL usept(L_PINT,L_NTREF) ! mask if pfref grid point will be used
142	INTEGER inflay(L_PINT) ! nearest inferior GCM layer for pfgasref grid points
143
144	!=======================================================================
145	! I. Initialization on every call
146	!=======================================================================
147
148
149	! How much light do we get ?
150	do nw=1,L_NSPECTV
151	stel(nw)=stellarf(nw)/(dist_star**2)
152	end do
153
154	! Convert (microphysical) tracers for optics: X.kg-1 --> X.m-2
155	! NOTE: it should be moved somewhere else: calmufi performs the same kind of
156	! computations... waste of time...
157	i2e(:,1:nlayer) = ( pplev(:,1:nlayer)-pplev(:,2:nlayer+1) ) / gzlat(:,1:nlayer)
158	pqmo(:,:,:) = 0.0
159	DO iq=1,nmicro
160	pqmo(:,:,iq) = pq(:,:,iq)*i2e(:,:)
161	ENDDO
162
163	! Default value for fixed species for whom vmr has been taken
164	! into account while computing high-resolution spectra
165	if (corrk_recombin) pqr(:,:,:) = 1.0
166
167	!-----------------------------------------------------------------------
168	do ig=1,ngrid ! Starting Big Loop over every GCM column
169	!-----------------------------------------------------------------------
170
171	! Recombine reference corr-k if needed
172	if (corrk_recombin) then
173
174	! NB : To have decent CPU time recombining is not done on all gridpoints and wavelenghts but we
175	! calculate a gasi/v_recomb variable on the reference corrk-k T,P grid (only for T,P values
176	! who match the atmospheric conditions ) which is then processed as a standard pre-mix in
177	! optci/v routines, but updated every time tracers on the ref P grid have varied > 1%.
178
179	! Extract tracers for variable radiative species
180	! Also find the nearest GCM layer under each ref pressure
181	do ip=1,L_PINT
182
183	ilay=0
184	found = .false.
185	do l=1,nlayer
186	if ( pplay(ig,l) .gt. 10.0**(pfgasref(ip)+2.0) ) then ! pfgasref=log(p[mbar])
187	found=.true.
188	ilay=l
189	endif
190	enddo
191
192	if (.not. found ) then ! set to min
193	do iq=1,L_REFVAR
194	if ( radvar_mask(iq) ) then
195	pqr(ig,ip,iq) = pq(ig,1,radvar_indx(iq)) / rat_mmol(radvar_indx(iq)-nmicro) ! mol/mol
196	endif
197	enddo
198	else
199	if (ilay==nlayer) then ! set to max
200	do iq=1,L_REFVAR
201	if ( radvar_mask(iq) ) then
202	pqr(ig,ip,iq) = pq(ig,nlayer,radvar_indx(iq)) / rat_mmol(radvar_indx(iq)-nmicro) ! mol/mol
203	endif
204	enddo
205	else ! standard
206	fact = ( 10.0**(pfgasref(ip)+2.0) - pplay(ig,ilay+1) ) / ( pplay(ig,ilay) - pplay(ig,ilay+1) ) ! pfgasref=log(p[mbar])
207	do iq=1,L_REFVAR
208	if ( radvar_mask(iq) ) then
209	pqr(ig,ip,iq) = pq(ig,ilay,radvar_indx(iq))*fact pq(ig,ilay+1,radvar_indx(iq))**(1.0-fact)
210	pqr(ig,ip,iq) = pqr(ig,ip,iq) / rat_mmol(radvar_indx(iq)-nmicro) ! mol/mol
211	endif
212	enddo
213	endif ! if ilay==nlayer
214	endif ! if not found
215
216	inflay(ip) = ilay
217
218	enddo ! ip=1,L_PINT
219
220	! NB : The following usept is a trick to call recombine only for the reference T-P
221	! grid points that are useful given the temperature range at this altitude
222	! It saves a looot of time - JVO 18
223	usept(:,:) = .true.
224	do ip=1,L_PINT-1
225	if ( inflay(ip+1)==nlayer ) then
226	usept(ip,:) = .false.
227	endif
228	if ( inflay(ip) == 0 ) then
229	usept(ip+1:,:) = .false.
230	endif
231	if ( usept(ip,1) ) then ! if not all false
232	tmin = minval(pt(ig,max(inflay(ip+1)+1,1):min(inflay(ip)+1,nlayer)))
233	tmax = maxval(pt(ig,max(inflay(ip+1)+1,1):min(inflay(ip)+1,nlayer)))
234	do it=1,L_NTREF-1
235	if ( tgasref(it+1) .lt. tmin ) then
236	usept(ip,it) = .false.
237	endif
238	enddo
239	do it=2,L_NTREF
240	if ( tgasref(it-1) .gt. tmax ) then
241	usept(ip,it) = .false.
242	endif
243	enddo
244	! in case of out-of-bounds
245	if ( tgasref(1) .lt. tmin ) usept(ip,1) = .true.
246	if ( tgasref(L_NTREF) .gt. tmax ) usept(ip,L_NTREF) = .true.
247	endif
248	enddo ! ip=1,L_PINT-1
249	! deal with last bound
250	if ( inflay(L_PINT-1).ne.0 ) usept(L_PINT,:) = usept(L_PINT-1,:)
251
252
253	do ip=1,L_PINT
254
255	! Recombine k at (useful only!) reference T-P values if tracers or T have enough varied
256	do it=1,L_NTREF
257
258	if ( usept(ip,it) .eqv. .false. ) cycle
259
260	do l=1,L_REFVAR
261	if ( abs( (pqr(ig,ip,l) - pqrold(ip,l)) / max(1.0e-30,pqrold(ip,l))) .GT. 0.01 & ! +- 1%
262	.or. ( useptold(ip,it) .eqv. .false. ) ) then ! in case T change but not the tracers
263	call recombin_corrk( pqr(ig,ip,:),ip,it )
264	exit ! one is enough to trigger the update
265	endif
266	enddo
267
268	enddo
269
270	enddo ! ip=1,L_PINT
271
272	useptold(:,:)=usept(:,:)
273
274	endif ! if corrk_recombin
275
276	!=======================================================================
277	! II. Transformation of the GCM variables
278	!=======================================================================
279
280
281	! Albedo and Emissivity.
282	albi=1-emis(ig) ! Long Wave.
283	DO nw=1,L_NSPECTV ! Short Wave loop.
284	albv(nw)=albedo(ig,nw)
285	ENDDO
286
287	if ((ngrid.eq.1).and.(global1d)) then ! Fixed zenith angle 'szangle' in 1D simulations w/ globally-averaged sunlight.
288	acosz = cos(pi*szangle/180.0)
289	print*,'acosz=',acosz,', szangle=',szangle
290	else
291	acosz=mu0(ig) ! Cosine of sun incident angle : 3D simulations or local 1D simulations using latitude.
292	endif
293
294	!-----------------------------------------------------------------------
295	! Pressure and temperature
296	!-----------------------------------------------------------------------
297
298	DO l=1,nlayer
299	plevrad(2*l) = pplay(ig,nlayer+1-l)/scalep
300	plevrad(2*l+1) = pplev(ig,nlayer+1-l)/scalep
301	tlevrad(2*l) = pt(ig,nlayer+1-l)
302	tlevrad(2*l+1) = (pt(ig,nlayer+1-l)+pt(ig,max(nlayer-l,1)))/2
303	END DO
304
305	plevrad(1) = 0.
306	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.
307
308	tlevrad(1) = tlevrad(2)
309	tlevrad(2*nlayer+1)=tsurf(ig)
310
311	pmid(1) = max(pgasmin,0.0001*plevrad(3))
312	pmid(2) = pmid(1)
313
314	tmid(1) = tlevrad(2)
315	tmid(2) = tmid(1)
316
317	DO l=1,L_NLAYRAD-1
318	tmid(2l+1) = tlevrad(2l+1)
319	tmid(2l+2) = tlevrad(2l+1)
320	pmid(2l+1) = plevrad(2l+1)
321	pmid(2l+2) = plevrad(2l+1)
322	END DO
323	pmid(L_LEVELS) = plevrad(L_LEVELS)
324	tmid(L_LEVELS) = tlevrad(L_LEVELS)
325
326	!!Alternative interpolation:
327	! pmid(3) = pmid(1)
328	! pmid(4) = pmid(1)
329	! tmid(3) = tmid(1)
330	! tmid(4) = tmid(1)
331	! DO l=2,L_NLAYRAD-1
332	! tmid(2l+1) = tlevrad(2l)
333	! tmid(2l+2) = tlevrad(2l)
334	! pmid(2l+1) = plevrad(2l)
335	! pmid(2l+2) = plevrad(2l)
336	! END DO
337	! pmid(L_LEVELS) = plevrad(L_LEVELS-1)
338	! tmid(L_LEVELS) = tlevrad(L_LEVELS-1)
339
340	! Test for out-of-bounds pressure.
341	if(plevrad(3).lt.pgasmin)then
342	print*,'Minimum pressure is outside the radiative'
343	print*,'transfer kmatrix bounds, exiting.'
344	call abort
345	elseif(plevrad(L_LEVELS).gt.pgasmax)then
346	print*,'Maximum pressure is outside the radiative'
347	print*,'transfer kmatrix bounds, exiting.'
348	call abort
349	endif
350
351	! Test for out-of-bounds temperature.
352	do k=1,L_LEVELS
353	if(tlevrad(k).lt.tgasmin)then
354	print*,'Minimum temperature is outside the radiative'
355	print*,'transfer kmatrix bounds'
356	print*,"k=",k," tlevrad(k)=",tlevrad(k)
357	print*,"tgasmin=",tgasmin
358	if (strictboundcorrk) then
359	call abort
360	else
361	print,'**********************************************'
362	print*,'we allow model to continue with tlevrad=tgasmin'
363	print*,' ... we assume we know what you are doing ... '
364	print*,' ... but do not let this happen too often ... '
365	print,'**********************************************'
366	!tlevrad(k)=tgasmin
367	endif
368	elseif(tlevrad(k).gt.tgasmax)then
369	! print*,'Maximum temperature is outside the radiative'
370	! print*,'transfer kmatrix bounds, exiting.'
371	! print*,"k=",k," tlevrad(k)=",tlevrad(k)
372	! print*,"tgasmax=",tgasmax
373	if (strictboundcorrk) then
374	call abort
375	else
376	! print,'**********************************************'
377	! print*,'we allow model to continue with tlevrad=tgasmax'
378	! print*,' ... we assume we know what you are doing ... '
379	! print*,' ... but do not let this happen too often ... '
380	! print,'**********************************************'
381	!tlevrad(k)=tgasmax
382	endif
383	endif
384
385	if (tlevrad(k).lt.tplanckmin) then
386	print*,'Minimum temperature is outside the boundaries for'
387	print*,'Planck function integration set in callphys.def, aborting.'
388	print*,"k=",k," tlevrad(k)=",tlevrad(k)
389	print*,"tplanckmin=",tplanckmin
390	message="Minimum temperature outside Planck function bounds - Change tplanckmin in callphys.def"
391	call abort_physic(subname,message,1)
392	else if (tlevrad(k).gt.tplanckmax) then
393	print*,'Maximum temperature is outside the boundaries for'
394	print*,'Planck function integration set in callphys.def, aborting.'
395	print*,"k=",k," tlevrad(k)=",tlevrad(k)
396	print*,"tplanckmax=",tplanckmax
397	message="Maximum temperature outside Planck function bounds - Change tplanckmax in callphys.def"
398	call abort_physic(subname,message,1)
399	endif
400
401	enddo
402
403	do k=1,L_NLAYRAD+1
404	if(tmid(k).lt.tgasmin)then
405	print*,'Minimum temperature is outside the radiative'
406	print*,'transfer kmatrix bounds, exiting.'
407	print*,"k=",k," tmid(k)=",tmid(k)
408	print*,"tgasmin=",tgasmin
409	if (strictboundcorrk) then
410	call abort
411	else
412	print,'**********************************************'
413	print*,'we allow model to continue with tmid=tgasmin'
414	print*,' ... we assume we know what you are doing ... '
415	print*,' ... but do not let this happen too often ... '
416	print,'**********************************************'
417	tmid(k)=tgasmin
418	endif
419	elseif(tmid(k).gt.tgasmax)then
420	! print*,'Maximum temperature is outside the radiative'
421	! print*,'transfer kmatrix bounds, exiting.'
422	! print*,"k=",k," tmid(k)=",tmid(k)
423	! print*,"tgasmax=",tgasmax
424	if (strictboundcorrk) then
425	call abort
426	else
427	! print,'**********************************************'
428	! print*,'we allow model to continue with tmid=tgasmin'
429	! print*,' ... we assume we know what you are doing ... '
430	! print*,' ... but do not let this happen too often ... '
431	! print,'**********************************************'
432	tmid(k)=tgasmax
433	endif
434	endif
435	enddo
436
437	!=======================================================================
438	! III. Calling the main radiative transfer subroutines
439	!=======================================================================
440
441	Cmk(:) = 0.01 * 1.0 / (gzlat(ig,:) * mugaz * 1.672621e-27) ! q_main=1.0 assumed.
442	gzlat_ig(:) = gzlat(ig,:)
443
444	! Compute the haze seasonal modulation factor
445	if (seashaze) call season_haze(zday,latitude(ig),plevrad,seashazefact)
446
447	!-----------------------------------------------------------------------
448	! Short Wave Part
449	!-----------------------------------------------------------------------
450
451	if(fract(ig) .ge. 1.0e-4) then ! Only during daylight.
452	if((ngrid.eq.1).and.(global1d))then
453	do nw=1,L_NSPECTV
454	stel_fract(nw)= stel(nw)* 0.25 / acosz ! globally averaged = divide by 4, and we correct for solar zenith angle
455	end do
456	else
457	do nw=1,L_NSPECTV
458	stel_fract(nw)= stel(nw) * fract(ig)
459	end do
460	endif
461
462	call optcv(pqmo(ig,:,:),nlayer,plevrad,tmid,pmid, &
463	dtauv,tauv,taucumv,wbarv,cosbv,tauray,taugsurf,seashazefact)
464
465	call sfluxv(dtauv,tauv,taucumv,albv,dwnv,wbarv,cosbv, &
466	acosz,stel_fract, &
467	nfluxtopv,fluxtopvdn,nfluxoutv_nu,nfluxgndv_nu, &
468	fmnetv,fluxupv,fluxdnv,fzerov,taugsurf)
469
470	else ! During the night, fluxes = 0.
471	nfluxtopv = 0.0d0
472	fluxtopvdn = 0.0d0
473	nfluxoutv_nu(:) = 0.0d0
474	nfluxgndv_nu(:) = 0.0d0
475	do l=1,L_NLAYRAD
476	fmnetv(l)=0.0d0
477	fluxupv(l)=0.0d0
478	fluxdnv(l)=0.0d0
479	end do
480	end if
481
482
483	! Equivalent Albedo Calculation (for OUTPUT). MT2015
484	if(fract(ig) .ge. 1.0e-4) then ! equivalent albedo makes sense only during daylight.
485	surface_stellar_flux=sum(nfluxgndv_nu(1:L_NSPECTV))
486	if(surface_stellar_flux .gt. 1.0e-3) then ! equivalent albedo makes sense only if the stellar flux received by the surface is positive.
487	DO nw=1,L_NSPECTV
488	albedo_temp(nw)=albedo(ig,nw)*nfluxgndv_nu(nw)
489	ENDDO
490	albedo_temp(1:L_NSPECTV)=albedo_temp(1:L_NSPECTV)/surface_stellar_flux
491	albedo_equivalent(ig)=sum(albedo_temp(1:L_NSPECTV))
492	else
493	albedo_equivalent(ig)=0.0 ! Spectrally Integrated Albedo not defined for non-irradiated grid points. So we arbitrary set the equivalent albedo to 0.
494	endif
495	else
496	albedo_equivalent(ig)=0.0 ! Spectrally Integrated Albedo not defined for non-irradiated grid points. So we arbitrary set the equivalent albedo to 0.
497	endif
498
499
500	!-----------------------------------------------------------------------
501	! Long Wave Part
502	!-----------------------------------------------------------------------
503
504	call optci(pqmo(ig,:,:),nlayer,plevrad,tlevrad,tmid,pmid, &
505	dtaui,taucumi,cosbi,wbari,taugsurfi,seashazefact)
506
507	call sfluxi(plevrad,tlevrad,dtaui,taucumi,ubari,albi, &
508	wnoi,dwni,cosbi,wbari,nfluxtopi,nfluxtopi_nu, &
509	fmneti,fluxupi,fluxdni,fluxupi_nu,fzeroi,taugsurfi)
510
511	!-----------------------------------------------------------------------
512	! Transformation of the correlated-k code outputs
513	! (into dtlw, dtsw, fluxsurf_lw, fluxsurf_sw, fluxtop_lw, fluxtop_sw)
514
515	! Flux incident at the top of the atmosphere
516	fluxtop_dn(ig)=fluxtopvdn
517
518	fluxtop_lw(ig) = real(nfluxtopi)
519	fluxabs_sw(ig) = real(-nfluxtopv)
520	fluxsurf_lw(ig) = real(fluxdni(L_NLAYRAD))
521	fluxsurf_sw(ig) = real(fluxdnv(L_NLAYRAD))
522
523	! Flux absorbed by the surface. By MT2015.
524	fluxsurfabs_sw(ig) = fluxsurf_sw(ig)*(1.-albedo_equivalent(ig))
525
526	if(fluxtop_dn(ig).lt.0.0)then
527	print*,'Achtung! fluxtop_dn has lost the plot!'
528	print*,'fluxtop_dn=',fluxtop_dn(ig)
529	print*,'acosz=',acosz
530	print*,'temp= ',pt(ig,:)
531	print*,'pplay= ',pplay(ig,:)
532	call abort
533	endif
534
535	! Spectral output, for exoplanet observational comparison
536	if(specOLR)then
537	do nw=1,L_NSPECTI
538	OLR_nu(ig,nw)=nfluxtopi_nu(nw)/DWNI(nw) !JL Normalize to the bandwidth
539	end do
540	do nw=1,L_NSPECTV
541	!GSR_nu(ig,nw)=nfluxgndv_nu(nw)
542	OSR_nu(ig,nw)=nfluxoutv_nu(nw)/DWNV(nw) !JL Normalize to the bandwidth
543	end do
544	endif
545
546	! Finally, the heating rates
547
548	DO l=2,L_NLAYRAD
549	dtsw(ig,L_NLAYRAD+1-l)=(fmnetv(l)-fmnetv(l-1)) &
550	gzlat(ig,L_NLAYRAD+1-l)/(cppscalep(plevrad(2l+1)-plevrad(2*l-1)))
551	dtlw(ig,L_NLAYRAD+1-l)=(fmneti(l)-fmneti(l-1)) &
552	gzlat(ig,L_NLAYRAD+1-l)/(cppscalep(plevrad(2l+1)-plevrad(2*l-1)))
553	END DO
554
555	! These are values at top of atmosphere
556	dtsw(ig,L_NLAYRAD)=(fmnetv(1)-nfluxtopv) &
557	gzlat(ig,L_NLAYRAD)/(cppscalep*(plevrad(3)-plevrad(1)))
558	dtlw(ig,L_NLAYRAD)=(fmneti(1)-nfluxtopi) &
559	gzlat(ig,L_NLAYRAD)/(cppscalep*(plevrad(3)-plevrad(1)))
560
561
562	! Optical thickness diagnostics (added by JVO)
563	if (diagdtau) then
564	do l=1,L_NLAYRAD
565	do nw=1,L_NSPECTV
566	int_dtauv(ig,l,nw) = 0.0d0
567	DO k=1,L_NGAUSS
568	! Output exp(-tau) because gweight ponderates exp and not tau itself
569	int_dtauv(ig,l,nw)= int_dtauv(ig,l,nw) + exp(-dtauv(l,nw,k))*gweight(k)
570	ENDDO
571	enddo
572	do nw=1,L_NSPECTI
573	int_dtaui(ig,l,nw) = 0.0d0
574	DO k=1,L_NGAUSS
575	! Output exp(-tau) because gweight ponderates exp and not tau itself
576	int_dtaui(ig,l,nw)= int_dtaui(ig,l,nw) + exp(-dtaui(l,nw,k))*gweight(k)
577	ENDDO
578	enddo
579	enddo
580	endif
581
582
583	!-----------------------------------------------------------------------
584	end do ! End of big loop over every GCM column.
585	!-----------------------------------------------------------------------
586
587
588	!-----------------------------------------------------------------------
589	! Additional diagnostics
590	!-----------------------------------------------------------------------
591
592	! IR spectral output, for exoplanet observational comparison
593	if(lastcall.and.(ngrid.eq.1))then ! could disable the 1D output, they are in the diagfi and diagspec... JL12
594
595	print*,'Saving scalar quantities in surf_vals.out...'
596	print*,'psurf = ', pplev(1,1),' Pa'
597	open(116,file='surf_vals.out')
598	write(116,*) tsurf(1),pplev(1,1),fluxtop_dn(1), &
599	real(-nfluxtopv),real(nfluxtopi)
600	close(116)
601
602
603	! USEFUL COMMENT - Do Not Remove.
604	!
605	! if(specOLR)then
606	! open(117,file='OLRnu.out')
607	! do nw=1,L_NSPECTI
608	! write(117,*) OLR_nu(1,nw)
609	! enddo
610	! close(117)
611	!
612	! open(127,file='OSRnu.out')
613	! do nw=1,L_NSPECTV
614	! write(127,*) OSR_nu(1,nw)
615	! enddo
616	! close(127)
617	! endif
618
619	! OLR vs altitude: do it as a .txt file.
620	OLRz=.false.
621	if(OLRz)then
622	print*,'saving IR vertical flux for OLRz...'
623	open(118,file='OLRz_plevs.out')
624	open(119,file='OLRz.out')
625	do l=1,L_NLAYRAD
626	write(118,) plevrad(2l)
627	do nw=1,L_NSPECTI
628	write(119,*) fluxupi_nu(l,nw)
629	enddo
630	enddo
631	close(118)
632	close(119)
633	endif
634
635	endif
636
637	if (lastcall) then
638	IF( ALLOCATED( gasi ) ) DEALLOCATE( gasi )
639	IF( ALLOCATED( gasv ) ) DEALLOCATE( gasv )
640	IF( ALLOCATED( gasi_recomb ) ) DEALLOCATE( gasi_recomb )
641	IF( ALLOCATED( gasv_recomb ) ) DEALLOCATE( gasv_recomb )
642	IF( ALLOCATED( pqrold ) ) DEALLOCATE( pqrold )
643	IF( ALLOCATED( useptold ) ) DEALLOCATE( useptold )
644	!$OMP BARRIER
645	!$OMP MASTER
646	IF( ALLOCATED( pgasref ) ) DEALLOCATE( pgasref )
647	IF( ALLOCATED( tgasref ) ) DEALLOCATE( tgasref )
648	IF( ALLOCATED( pfgasref ) ) DEALLOCATE( pfgasref )
649	IF( ALLOCATED( gweight ) ) DEALLOCATE( gweight )
650	!$OMP END MASTER
651	!$OMP BARRIER
652	endif
653
654
655	end subroutine callcorrk

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