SUBROUTINE JVALUE(K) INCLUDE 'PARAMETERS.INC' COMMON & /BLOCK1/ NDISSC & /BLOCK7/ RATE(IB,NALT) & /BLOCK8/ IPHOTO(IB) , LAST(IB) , & LOW(IB) , SIGMA(NWAVE,IB) & /BLOCK19/ TRANS(NWAVE,NALT) & /ONED35/ FLUX(NWAVE) C THIS SUBROUTINE COMPUTES THE JVALUES DO I = 1 , NDISSC IP = IPHOTO(I) IF (IPHOTO(I).eq.0) GO TO 555 IF ( (IP .NE. 0) .AND. & (LAST(IP) .NE. 0 ) ) THEN ! SKIP PHOTOLYSIS BELOW ! LYMAN ALPHA L1 = LOW( IP ) L2 = LAST( IP ) C USE MIDPOINT RULE TO NUMERICALLY INTEGRATE THE PHOTODISSOCIATION C INTEGRAL C CALCULATE PORTION BELOW SRB RJ = 0.0D0 DO LAMBDA = L1 , LYMAN + 10 RJ = RJ + FLUX(LAMBDA)* & SIGMA(LAMBDA,IP)* & TRANS(LAMBDA,K) ENDDO C ADD ON SRB CONTRIBUTION (IF ANY) IF( (L1 .LE. LYMAN+16) .AND. & (L2 .GE. LYMAN+11) )THEN RJ = RJ + RJSRB(I,K) ENDIF C ADD ON PORTION BEYOND SRB DO LAMBDA = LYMAN + 17 , L2 RJ = RJ + FLUX(LAMBDA)* & SIGMA(LAMBDA,IP)* & TRANS(LAMBDA,K) ENDDO RATE(I,K) = RJ ENDIF 555 ENDDO RETURN END C------------------------------------------------------------------------------- C------------------------------------------------------------------------------- C------------------------------------------------------------------------------- SUBROUTINE RJAVG INCLUDE 'PARAMETERS.INC' INCLUDE 'PLANET.INC' COMMON & /SWITCHES/ ZLAT , DELTAT , DELT1 , DAYSTART , & TIMESTART , TIMESTOP , OUTTIME , & MODE , NTIME , NITER , IDIFF , istepdump & /BLOCK6/ MCROSS(MB) & /BLOCK12/ CROSS(NWAVE,MB) & /BLOCK14/ MTAU(MB) & /BLOCK16/ COSSZA(NTRAP) & /BLOCK17/ NANGLE(NALT) & /BLOCK19/ TRANS(NWAVE,NALT) & /BLOCK30/ NPI2 & /ONED46/ COLUMN(NTRAP,NALT,MB) & /BLOCK41/ S(NTRAP,NWAVE,NALT) C THIS SUBROUTINE COMPUTES THE DIURNAL AVERAGE OF EXP(-TAU). IT CAN BE RUN C IN TWO MODES. SETTING ISPHERE = 0 PRODUCES A PLANE-PARALLEL ATMOSPHERE. THIS C MODE DIFFERS FROM THE SECANT APPROXIMATION IN THAT THE DIFFERENTIAL C SLANT PATH IS APPROXIMATED BY A MORE ACCURATE FORMULA FOR HIGH SOLAR C ZENITH ANGLES ( THE SECANT BLOWS UP WHEN CHI = PI/2 ). SETTING ISPHERE = 1 C PRODUCES THE FULL RAY-TRACE CALCULATION FOR A SPHERICAL ATMOSPHERE. C COMPUTE OPTICAL DEPTHS FOR SZA < 90 DEGREES C CALCULATE DIFFERENTIAL OPTICAL DEPTH AT KTH LAYER DO K = 1 , NALT DO NANG = 1 , NPI2 COL1 = COLUMN(NANG,K,MTAU(1)) COL2 = COLUMN(NANG,K,MTAU(2)) COL3 = COLUMN(NANG,K,MTAU(3)) DO LAMBDA = 1 , NWAVE TAU = COL1*CROSS(LAMBDA,MCROSS(1)) + & COL2*CROSS(LAMBDA,MCROSS(2)) + & COL3*CROSS(LAMBDA,MCROSS(3)) S(NANG,LAMBDA,K) = DEXP(-TAU) ENDDO ENDDO ENDDO IF( ISPHERE .EQ. 1 ) THEN DO K = 1 , NALT N1 = NPI2 + 1 N2 = NANGLE(K) DO NANG = N1 , N2 COL1 = COLUMN(NANG,K,MTAU(1)) COL2 = COLUMN(NANG,K,MTAU(2)) COL3 = COLUMN(NANG,K,MTAU(3)) DO LAMBDA = 1 , NWAVE TAU = COL1*CROSS(LAMBDA,MCROSS(1)) + & COL2*CROSS(LAMBDA,MCROSS(2)) + & COL3*CROSS(LAMBDA,MCROSS(3)) S(NANG,LAMBDA,K) = DEXP(-TAU) ENDDO ENDDO ENDDO ENDIF ! END RAY-TRACE COMPUTATIONS IF( IDIFF .EQ. 1 ) THEN CALL ALBAVG ! ADD GROUND ALBEDO ONTO S CALL MSAVG ! MULTIPLE SCATTERING CONTRIBUTION ENDIF C############################################################################ C CALCULATE DIURNAL AVERAGE OF EXP(-TAU) C USE TRAPEZOIDAL RULE TO DO TIME INTEGRATION DO K = 1 , NALT IF( ISPHERE .EQ. 1 ) THEN NEND = NANGLE(K) - 1 ELSE NEND = NPI2 - 1 ENDIF DO LAMBDA = 1 , NWAVE SUM = 0.0D0 DO NANG = 1 , NEND SUM = SUM + 0.5D0*(S(NANG,LAMBDA,K) + S(NANG+1,LAMBDA,K)) ENDDO IF( NEND .EQ. 0 ) THEN ! SPECIAL CASE SUM = 0.5D0*S(1,LAMBDA,K) ENDIF TRANS(LAMBDA,K) = SUM/(NTRAP-1.0) ENDDO ENDDO RETURN END C------------------------------------------------------------------------------- C------------------------------------------------------------------------------- C------------------------------------------------------------------------------- SUBROUTINE RJDIURN INCLUDE 'PARAMETERS.INC' INCLUDE 'PLANET.INC' COMMON & /SWITCHES/ ZLAT , DELTAT , DELT1 , DAYSTART , & TIMESTART , TIMESTOP , OUTTIME , & MODE , NTIME , NITER , IDIFF , istepdump & /BLOCK6/ MCROSS(MB) & /BLOCK12/ CROSS(NWAVE,MB) & /BLOCK14/ MTAU(MB) & /BLOCK19/ TRANS(NWAVE,NALT) & /BLOCK27/ PI & /ONED15/ THOUR & /ONED32/ SUNRISE(NALT) , SUNSET(NALT) & /ONED41/ SZA & /ONED47/ COLUMN(NALT,MB) C THIS SUBROUTINE COMPUTES EXP(-TAU). IT CAN BE RUN IN TWO MODES. C SETTING ISPHERE = 0 PRODUCES A PLANE-PARALLEL ATMOSPHERE. THIS C MODE DIFFERS FROM THE SECANT APPROXIMATION IN THAT THE DIFFERENTIAL C SLANT PATH IS APPROXIMATED BY A MORE ACCURATE FORMULA FOR HIGH SOLAR C ZENITH ANGLES ( THE SECANT BLOWS UP WHEN CHI = PI/2 ). SETTING ISPHERE = 1 C PRODUCES THE FULL RAY-TRACE CALCULATION FOR A SPHERICAL ATMOSPHERE. C COMPUTE OPTICAL DEPTH USING SIMPLIFIED CALCULATIONS FOR SZA < 90 DEGREES IF( SZA .LE. PI/2.0 ) THEN DO K = 1 , NALT COL1 = COLUMN(K,MTAU(1)) COL2 = COLUMN(K,MTAU(2)) COL3 = COLUMN(K,MTAU(3)) DO LAMBDA = 1 , NWAVE TAU = COL1*CROSS(LAMBDA,MCROSS(1)) + & COL2*CROSS(LAMBDA,MCROSS(2)) + & COL3*CROSS(LAMBDA,MCROSS(3)) TRANS(LAMBDA,K) = DEXP(-TAU) ENDDO ENDDO IF( IDIFF .EQ. 1 ) THEN CALL ALBDIU ! ADD GROUND ALBEDO ONTO TRANS CALL MSDIU ! INCLUDE MULTIPLE SCATTERING CONTRIBUTION ENDIF ENDIF ! END SZA < 90 C CALCULATE OPTICAL DEPTHS FOR SOLAR ZENITH ANGLES > PI/2. THE COLUMN DEPTH IS C COMPUTED BY SUBTRACTING THE COLUMN DEPTH AT ANGLE PI - CHI FROM TWICE THE C COLUMND DEPTH TO THE TANGENT POINT. IF( (SZA .GT. PI/2.0) .AND. (ISPHERE .EQ. 1) ) THEN DO K = 1 , NALT IF( (THOUR .GE. SUNRISE(K)) .AND. & (THOUR .LT. SUNSET(K)) )THEN COL1 = COLUMN(K,MTAU(1)) COL2 = COLUMN(K,MTAU(2)) COL3 = COLUMN(K,MTAU(3)) DO LAMBDA = 1 , NWAVE TAU = COL1*CROSS(LAMBDA,MCROSS(1)) + & COL2*CROSS(LAMBDA,MCROSS(2)) + & COL3*CROSS(LAMBDA,MCROSS(3)) TRANS(LAMBDA,K) = DEXP(-TAU) ENDDO ELSE DO LAMBDA = 1 , NWAVE TRANS(LAMBDA,K) = 0.0D0 ! IN DARKNESS ENDDO ENDIF ENDDO ! END LOOP OVER K ENDIF ! END SZA > 90 (SPHERICAL CASE) IF( (SZA .GT. PI/2.0) .AND. (ISPHERE .EQ. 0) ) THEN DO K = 1 , NALT DO LAMBDA = 1 , NWAVE TRANS(LAMBDA,K) = 0.0D0 ENDDO ENDDO ENDIF ! (NON-SPHERICAL CASE) RETURN END