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optcv.F90 @ 2050

Last change on this file since 2050 was 2050, checked in by jvatant, 6 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: 13.6 KB

Line
1	SUBROUTINE OPTCV(PQMO,NLAY,PLEV,TMID,PMID, &
2	DTAUV,TAUV,TAUCUMV,WBARV,COSBV,TAURAY,TAUGSURF,SEASHAZEFACT)
3
4	use radinc_h
5	use radcommon_h, only: gasv,gasv_recomb,tlimit,Cmk,gzlat_ig, &
6	tgasref,pfgasref,wnov,scalep,indv,gweight
7	use gases_h
8	use comcstfi_mod, only: r
9	use callkeys_mod, only: continuum,graybody,callgasvis,corrk_recombin, &
10	callclouds,callmufi,seashaze,uncoupl_optic_haze
11	use tracer_h, only: nmicro,nice
12	use MMP_OPTICS
13
14	implicit none
15
16	!==================================================================
17	!
18	! Purpose
19	! -------
20	! Calculates shortwave optical constants at each level.
21	!
22	! Authors
23	! -------
24	! Adapted from the NASA Ames code by R. Wordsworth (2009)
25	! Clean and adaptation to Titan by J. Vatant d'Ollone (2016-17)
26	!
27	!==================================================================
28	!
29	! THIS SUBROUTINE SETS THE OPTICAL CONSTANTS IN THE VISUAL
30	! IT CALCULATES FOR EACH LAYER, FOR EACH SPECTRAL INTERVAL IN THE VISUAL
31	! LAYER: WBAR, DTAU, COSBAR
32	! LEVEL: TAU
33	!
34	! TAUV(L,NW,NG) is the cumulative optical depth at the top of radiation code
35	! layer L. NW is spectral wavelength interval, ng the Gauss point index.
36	!
37	! TLEV(L) - Temperature at the layer boundary
38	! PLEV(L) - Pressure at the layer boundary (i.e. level)
39	! GASV(NT,NPS,NW,NG) - Visible k-coefficients
40	!
41	!-------------------------------------------------------------------
42
43
44	!==========================================================
45	! Input/Output
46	!==========================================================
47	REAL*8, INTENT(IN) :: PQMO(nlay,nmicro) ! Tracers for microphysics optics (X/m2).
48	INTEGER, INTENT(IN) :: NLAY ! Number of pressure layers (for pqmo)
49	REAL*8, INTENT(IN) :: PLEV(L_LEVELS)
50	REAL*8, INTENT(IN) :: TMID(L_LEVELS), PMID(L_LEVELS)
51	REAL*8, INTENT(IN) :: TAURAY(L_NSPECTV)
52	REAL*8, INTENT(IN) :: SEASHAZEFACT(L_LEVELS)
53
54	REAL*8, INTENT(OUT) :: DTAUV(L_NLAYRAD,L_NSPECTV,L_NGAUSS)
55	REAL*8, INTENT(OUT) :: TAUV(L_NLEVRAD,L_NSPECTV,L_NGAUSS)
56	REAL*8, INTENT(OUT) :: TAUCUMV(L_LEVELS,L_NSPECTV,L_NGAUSS)
57	REAL*8, INTENT(OUT) :: COSBV(L_NLAYRAD,L_NSPECTV,L_NGAUSS)
58	REAL*8, INTENT(OUT) :: WBARV(L_NLAYRAD,L_NSPECTV,L_NGAUSS)
59	REAL*8, INTENT(OUT) :: TAUGSURF(L_NSPECTV,L_NGAUSS-1)
60	! ==========================================================
61
62	real*8 DTAUKV(L_LEVELS,L_NSPECTV,L_NGAUSS)
63
64	! Titan customisation
65	! J. Vatant d'Ollone (2016)
66	real*8 DHAZE_T(L_LEVELS,L_NSPECTI)
67	real*8 DHAZES_T(L_LEVELS,L_NSPECTI)
68	real*8 SSA_T(L_LEVELS,L_NSPECTI)
69	real*8 ASF_T(L_LEVELS,L_NSPECTI)
70	real*8 INT_DTAU(L_NLAYRAD,L_NSPECTI)
71	real*8 K_HAZE(L_NLAYRAD,L_NSPECTI)
72
73	CHARACTER*2 str2
74	! ==========================
75
76	integer L, NW, NG, K, LK, IAER
77	integer MT(L_LEVELS), MP(L_LEVELS), NP(L_LEVELS)
78	real*8 ANS, TAUGAS
79	real*8 TRAY(L_LEVELS,L_NSPECTV)
80	real*8 DPR(L_LEVELS), U(L_LEVELS)
81	real*8 LCOEF(4), LKCOEF(L_LEVELS,4)
82
83	real*8 DCONT
84	real*8 DRAYAER
85	double precision wn_cont, p_cont, p_air, T_cont, dtemp, dtempc
86	double precision p_cross
87
88	real*8 KCOEF(4)
89
90	! temporary variable to reduce memory access time to gasv
91	real*8 tmpk(2,2)
92
93	! temporary variables for multiple aerosol calculation
94	real*8 atemp(L_NLAYRAD,L_NSPECTV)
95	real*8 btemp(L_NLAYRAD,L_NSPECTV)
96	real*8 ctemp(L_NLAYRAD,L_NSPECTV)
97
98	! variables for k in units m^-1
99	real*8 dz(L_LEVELS)
100
101	integer igas, jgas, ilay
102
103	integer interm
104
105	real*8 m0as,m3as,m0af,m3af
106	real*8 ext_s,sca_s,ssa_s,asf_s
107	real*8 ext_f,sca_f,ssa_f,asf_f
108	logical,save :: firstcall=.true.
109	!$OMP THREADPRIVATE(firstcall)
110
111
112	!! AS: to save time in computing continuum (see bilinearbig)
113	IF (.not.ALLOCATED(indv)) THEN
114	ALLOCATE(indv(L_NSPECTV,ngasmx,ngasmx))
115	indv = -9999 ! this initial value means "to be calculated"
116	ENDIF
117
118	! Some initialisation beacause there's a pb with disr_haze at the limits (nw=1)
119	! I should check this - For now we set vars to zero : better than nans - JVO 2017
120
121	dhaze_t(:,:) = 0.
122	ssa_t(:,:) = 0.
123	asf_t(:,:) = 0.
124
125
126	!=======================================================================
127	! Determine the total gas opacity throughout the column, for each
128	! spectral interval, NW, and each Gauss point, NG.
129	! Calculate the continuum opacities, i.e., those that do not depend on
130	! NG, the Gauss index.
131
132	taugsurf(:,:) = 0.0
133	dpr(:) = 0.0
134	lkcoef(:,:) = 0.0
135
136	do K=2,L_LEVELS
137
138	ilay = k / 2 ! int. arithmetic => gives the gcm layer index
139
140	DPR(k) = PLEV(K)-PLEV(K-1)
141
142	! if we have continuum opacities, we need dz
143
144	dz(k) = dpr(k)RTMID(K)/(gzlat_ig(ilay)*PMID(K))
145	U(k) = Cmk(ilay)*DPR(k) ! only Cmk line in optcv.F
146
147	call tpindex(PMID(K),TMID(K),pfgasref,tgasref,LCOEF,MT(K),MP(K))
148
149	do LK=1,4
150	LKCOEF(K,LK) = LCOEF(LK)
151	end do
152	end do ! levels
153
154	! Rayleigh scattering
155	do NW=1,L_NSPECTV
156	do K=2,L_LEVELS
157	TRAY(K,NW) = TAURAY(NW) * DPR(K)
158	end do ! levels
159	end do
160
161	! we ignore K=1...
162	do K=2,L_LEVELS
163
164	ilay = k / 2 ! int. arithmetic => gives the gcm layer index
165
166	do NW=1,L_NSPECTV
167
168	! Optical coupling of YAMMS is plugged but inactivated (if false) for now
169	! as long as the microphysics only isn't fully debugged -- JVO 01/18
170	IF (callmufi .AND. (.NOT. uncoupl_optic_haze)) THEN
171	m0as = pqmo(ilay,1)
172	m3as = pqmo(ilay,2)
173	m0af = pqmo(ilay,3)
174	m3af = pqmo(ilay,4)
175
176	IF (.NOT.mmp_sph_optics_vis(m0as,m3as,nw,ext_s,sca_s,ssa_s,asf_s)) &
177	CALL abort_gcm("optcv", "Fatal error in mmp_sph_optics_vis", 12)
178	IF (.NOT.mmp_fra_optics_vis(m0af,m3af,nw,ext_f,sca_f,ssa_f,asf_f)) &
179	CALL abort_gcm("optcv", "Fatal error in mmp_fra_optics_vis", 12)
180	dhaze_T(k,nw) = ext_s+ext_f
181	SSA_T(k,nw) = (sca_s+sca_f)/dhaze_T(k,nw)
182	ASF_T(k,nw) = (asf_ssca_s + asf_fsca_f) /(sca_s+sca_f)
183	IF (callclouds.and.firstcall) &
184	WRITE(,) 'WARNING: In optcv, optical properties &
185	&calculations are not implemented yet'
186	ELSE
187	! Call fixed vertical haze profile of extinction - same for all columns
188	call disr_haze(dz(k),plev(k),wnov(nw),dhaze_T(k,nw),SSA_T(k,nw),ASF_T(k,nw))
189	if (seashaze) dhaze_T(k,nw) = dhaze_T(k,nw)*seashazefact(k)
190	ENDIF
191
192	DRAYAER = TRAY(K,NW)
193	! DRAYAER is Tau RAYleigh scattering, plus AERosol opacity
194	DRAYAER = DRAYAER + DHAZE_T(K,NW) ! Titan's aerosol
195
196	DCONT = 0.0 ! continuum absorption
197
198	if(continuum.and.(.not.graybody).and.callgasvis)then
199	! include continua if necessary
200	wn_cont = dble(wnov(nw))
201	T_cont = dble(TMID(k))
202	do igas=1,ngasmx
203
204	p_cont = dble(PMID(k)scalepgfrac(igas,ilay))
205
206	dtemp=0.0
207	if(igas.eq.igas_N2)then
208
209	interm = indv(nw,igas,igas)
210	! call interpolateN2N2(wn_cont,T_cont,p_cont,dtemp,.false.,interm)
211	indv(nw,igas,igas) = interm
212	! only goes to 500 cm^-1, so unless we're around a cold brown dwarf, this is irrelevant in the visible
213
214	elseif(igas.eq.igas_H2)then
215
216	! first do self-induced absorption
217	interm = indv(nw,igas,igas)
218	call interpolateH2H2(wn_cont,T_cont,p_cont,dtemp,.false.,interm)
219	indv(nw,igas,igas) = interm
220
221	! then cross-interactions with other gases
222	do jgas=1,ngasmx
223	p_cross = dble(PMID(k)scalepgfrac(jgas,ilay))
224	dtempc = 0.0
225	if(jgas.eq.igas_N2)then
226	interm = indv(nw,igas,jgas)
227	call interpolateN2H2(wn_cont,T_cont,p_cross,p_cont,dtempc,.false.,interm)
228	indv(nw,igas,jgas) = interm
229	! should be irrelevant in the visible
230	endif
231	dtemp = dtemp + dtempc
232	enddo
233
234	elseif(igas.eq.igas_CH4)then
235
236	! first do self-induced absorption
237	interm = indv(nw,igas,igas)
238	call interpolateCH4CH4(wn_cont,T_cont,p_cont,dtemp,.false.,interm)
239	indv(nw,igas,igas) = interm
240
241	! then cross-interactions with other gases
242	do jgas=1,ngasmx
243	p_cross = dble(PMID(k)scalepgfrac(jgas,ilay))
244	dtempc = 0.0
245	if(jgas.eq.igas_N2)then
246	interm = indv(nw,igas,jgas)
247	call interpolateN2CH4(wn_cont,T_cont,p_cross,p_cont,dtempc,.false.,interm)
248	indv(nw,igas,jgas) = interm
249	endif
250	dtemp = dtemp + dtempc
251	enddo
252
253	endif
254
255	DCONT = DCONT + dtemp
256
257	enddo
258
259	DCONT = DCONT*dz(k)
260
261	endif
262
263	do ng=1,L_NGAUSS-1
264
265	! Now compute TAUGAS
266
267	! JVO 2017 : added tmpk because the repeated calls to gasi/v increased dramatically
268	! the execution time of optci/v -> ~ factor 2 on the whole radiative
269	! transfer on the tested simulations !
270
271	if (corrk_recombin) then
272	tmpk = GASV_RECOMB(MT(K):MT(K)+1,MP(K):MP(K)+1,NW,NG)
273	else
274	tmpk = GASV(MT(K):MT(K)+1,MP(K):MP(K)+1,1,NW,NG)
275	endif
276
277	KCOEF(1) = tmpk(1,1) ! KCOEF(1) = GASV(MT(K),MP(K),1,NW,NG)
278	KCOEF(2) = tmpk(1,2) ! KCOEF(2) = GASV(MT(K),MP(K)+1,1,NW,NG)
279	KCOEF(3) = tmpk(2,2) ! KCOEF(3) = GASV(MT(K)+1,MP(K)+1,1,NW,NG)
280	KCOEF(4) = tmpk(2,1) ! KCOEF(4) = GASV(MT(K)+1,MP(K),1,NW,NG)
281
282	! Interpolate the gaseous k-coefficients to the requested T,P values
283
284	ANS = LKCOEF(K,1)KCOEF(1) + LKCOEF(K,2)KCOEF(2) + &
285	LKCOEF(K,3)KCOEF(3) + LKCOEF(K,4)KCOEF(4)
286
287
288	TAUGAS = U(k)*ANS
289
290	TAUGSURF(NW,NG) = TAUGSURF(NW,NG) + TAUGAS + DCONT
291	DTAUKV(K,nw,ng) = TAUGAS &
292	+ DRAYAER & ! DRAYAER includes all scattering contributions
293	+ DCONT ! For parameterized continuum aborption
294
295	end do
296
297	! Now fill in the "clear" part of the spectrum (NG = L_NGAUSS),
298	! which holds continuum opacity only
299
300	NG = L_NGAUSS
301	DTAUKV(K,nw,ng) = DRAYAER + DCONT ! Scattering + parameterized continuum absorption, including Titan's haze
302
303	end do
304	end do
305
306
307	!=======================================================================
308	! Now the full treatment for the layers, where besides the opacity
309	! we need to calculate the scattering albedo and asymmetry factors
310	! ======================================================================
311
312	! Haze scattering
313	DO NW=1,L_NSPECTV
314	DO K=2,L_LEVELS
315	DHAZES_T(K,NW) = DHAZE_T(K,NW) * SSA_T(K,NW) ! effect of scattering albedo on haze
316	ENDDO
317	ENDDO
318
319
320	DO NW=1,L_NSPECTV
321	DO L=1,L_NLAYRAD-1
322	K = 2*L+1
323	atemp(L,NW) = ASF_T(K,NW)DHAZES_T(K,NW) + ASF_T(K+1,NW)DHAZES_T(K+1,NW)
324	btemp(L,NW) = DHAZES_T(K,NW) + DHAZES_T(K+1,NW)
325	ctemp(L,NW) = btemp(L,NW) + 0.9999*(TRAY(K,NW) + TRAY(K+1,NW)) ! JVO 2017 : does this 0.999 is really meaningful ?
326	btemp(L,NW) = btemp(L,NW) + TRAY(K,NW) + TRAY(K+1,NW)
327	COSBV(L,NW,1:L_NGAUSS) = atemp(L,NW)/btemp(L,NW)
328	END DO ! L vertical loop
329
330	! Last level
331	L = L_NLAYRAD
332	K = 2*L+1
333	atemp(L,NW) = ASF_T(K,NW)*DHAZES_T(K,NW)
334	btemp(L,NW) = DHAZES_T(K,NW)
335	ctemp(L,NW) = btemp(L,NW) + 0.9999*TRAY(K,NW) ! JVO 2017 : does this 0.999 is really meaningful ?
336	btemp(L,NW) = btemp(L,NW) + TRAY(K,NW)
337	COSBV(L,NW,1:L_NGAUSS) = atemp(L,NW)/btemp(L,NW)
338
339
340	END DO ! NW spectral loop
341
342	DO NG=1,L_NGAUSS
343	DO NW=1,L_NSPECTV
344	DO L=1,L_NLAYRAD-1
345
346	K = 2*L+1
347	DTAUV(L,nw,ng) = DTAUKV(K,NW,NG) + DTAUKV(K+1,NW,NG)
348	WBARV(L,nw,ng) = ctemp(L,NW) / DTAUV(L,nw,ng)
349
350	END DO ! L vertical loop
351
352	! Last level
353
354	L = L_NLAYRAD
355	K = 2*L+1
356	DTAUV(L,nw,ng) = DTAUKV(K,NW,NG)
357
358	WBARV(L,NW,NG) = ctemp(L,NW) / DTAUV(L,NW,NG)
359
360	END DO ! NW spectral loop
361	END DO ! NG Gauss loop
362
363	! Total extinction optical depths
364
365	DO NG=1,L_NGAUSS ! full gauss loop
366	DO NW=1,L_NSPECTV
367	TAUV(1,NW,NG)=0.0D0
368	DO L=1,L_NLAYRAD
369	TAUV(L+1,NW,NG)=TAUV(L,NW,NG)+DTAUV(L,NW,NG)
370	END DO
371
372	TAUCUMV(1,NW,NG)=0.0D0
373	DO K=2,L_LEVELS
374	TAUCUMV(K,NW,NG)=TAUCUMV(K-1,NW,NG)+DTAUKV(K,NW,NG)
375	END DO
376	END DO
377	END DO ! end full gauss loop
378
379
380	! Titan's outputs (JVO, 2016)===============================================
381	! do l=1,L_NLAYRAD
382	! do nw=1,L_NSPECTV
383	! INT_DTAU(L,NW) = 0.0d+0
384	! DO NG=1,L_NGAUSS
385	! INT_DTAU(L,NW)= INT_DTAU(L,NW) + dtauv(L,nw,ng)*gweight(NG)
386	! enddo
387	! enddo
388	! enddo
389
390	! do nw=1,L_NSPECTV
391	! write(str2,'(i2.2)') nw
392	! call writediagfi(1,'kgv'//str2,'Gaz extinction coefficient VI band '//str2,'m-1',1,int_dtau(L_NLAYRAD:1:-1,nw)/dz_lay(L_NLAYRAD:1:-1))
393	! call writediagfi(1,'khv'//str2,'Haze extinction coefficient VI band '//str2,'m-1',1,k_haze(L_NLAYRAD:1:-1,nw)/dz_lay(L_NLAYRAD:1:-1))
394	! enddo
395
396	! ==============================================================================
397
398	if(firstcall) firstcall = .false.
399
400	return
401
402
403	end subroutine optcv

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