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callcorrk.F90 @ 2054

Last change on this file since 2054 was 2050, checked in by jvatant, 7 years ago

Major radiative transfer contribution : Add the 'corrk_recombin' option that allows to use
correlated-k for single species instead of pre-mix and enables more flexiblity for variable species.
-> Algorithm inspired from Lacis and Oinas 1991 and Amundsen et al 2016

+ Added 'recombin_corrk.F90' - Important improvements in 'sugas_corrk.90' and 'callcork.F90'

Must have the desired variable species as tracers -> TBD : Enable to force composition even if no tracers

To have decent CPU time recombining is not done on all gridpoints and wavelenghts but we calculate a gasi/v_recomb variable on the reference corrk-k T,P grid (only for T,P values who match the atmospheric conditions ) which is then processed as a standard pre-mix in optci/v routines, but updated every time tracers on the ref P grid have varied > 1%.

READ CAREFULY :

In case of 'corrk_recombin', the variable L_NREFVAR doesn't have the same meaning as before and doesn't stand for the different mixing ratios but the different species.
Input corr-k should be found in corrkdir within 'corrk_gcm_IR/VI_XXX.dat' and can contain a 'fixed' specie ( compulsory if you include self-broadening ) that MUST have been created with correct mixing ratios, or a variable specie for which mixing ratio MUST have been set to 1 ( no self-broadening then, assume it's a trace sepecie ) -> You can't neither have CIA of variable species included upstream in the corr-k

Property svn:executable set to *

File size: 25.4 KB

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

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