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/* This file is part of Cloudy and is copyright (C)1978-2008 by Gary J. Ferland and
 * others.  For conditions of distribution and use see copyright notice in license.txt */
/*ParseCosmicRays parse the cosmic rays command */
#include "cddefines.h"
#include "optimize.h"
#include "hextra.h"
#include "ionbal.h"
#include "input.h"
#include "parse.h"

/*ParseCosmicRays parse the cosmic rays command */
void ParseCosmicRays( char *chCard )
{
        long int i;
        bool lgEOL;
        realnum a;
        double var;

        DEBUG_ENTRY( "ParseCosmicRays()" );

        /* cosmic ray density, log of rate relative to background, log of H0 rate in neutral gas,
         * or density of rel. electrons,
         * quantity is log unless keyword linear appears */
        i = 5;
        /* if no number is present FFmtRead returns zero */
        a = (realnum)FFmtRead(chCard,&i,INPUT_LINE_LENGTH,&lgEOL);
        if( lgEOL )
                a = 0.;

        /* if keyword LINEAR not present, then log, and make linear */
        if( !nMatch("LINE",chCard) )
                a = (realnum)pow((realnum)10.f,a);
        /* a is now linear scale factor, or linear density, with default of 1 if no number  */

        /* default is cosmic ray ionization rate relative to galactic background, but can
         * also give density, which was the only option originally */
        if( nMatch("DENS",chCard) )
        {
                if( lgEOL )
                {
                        fprintf(ioQQQ,
                                " Either the log of the cosmic ray density must appear when density given.\n");
                        NoNumb(chCard);
                }
                hextra.cryden = a;

                /*  optional power law density  */
                hextra.crpowr = (realnum)FFmtRead(chCard,&i,INPUT_LINE_LENGTH,&lgEOL);

                /*  option to specify a temp for non-rel electrons - but only when a density */
                hextra.crtemp = (realnum)FFmtRead(chCard,&i,INPUT_LINE_LENGTH,&lgEOL);
                if( lgEOL )
                {
                        /* relativistic limit (Balbus and McKee) */
                        hextra.crtemp = 2.6e9;
                }
                else
                {
                        var = pow((realnum)10.f,hextra.crtemp);
                        hextra.crtemp = (realnum)MIN2(var,2.6e9);
                }
        }
        else if( nMatch( "RATE" , chCard ) )
        {
                /* this sets rate - use stored density and rate for background to set
                 * new density since code works with density */
                ASSERT( a > 0. );
                hextra.cryden = hextra.background_density * a / hextra.background_rate;
                hextra.crtemp = 2.6e9f;
        }
        else if( nMatch( "BACK" , chCard ) && nMatch( "GROU" , chCard ) )
        {
                /* >>chng 06 may 28, require explicit BACKGROUnd to hit background for safety */
                /* cr relative to galactic background BACK - no check on string since default */
                /* >>chng 04 mar 10, background is now 
                 * >>refer      cr      ion     Williams, J.P., Bergin, E.A., Caseli, P., Myers, P.C., & Plume, R. 1998, ApJ, 503, 689 */
                /* galactic background cosmic ray density to produce
                 * secondary ionization rate quoted by Tielens and Hollenbach */
                /* hextra.cryden = 2e-9f;*/
                /* >>chng 99 jun 24, slight change to value
                 * quoted by 
                 * >>refer      cosmic ray      ionization rate McKee, C.M., 1999, astro-ph 9901370
                 * this will produce a total
                 * secondary ionization rate of 2.5e-17 s^-1, as tested in 
                 * tsuite secondary.in.  If each ionization produces 2.4 eV of heat,
                 * the background heating rate should be 9.6e-29 * n*/
                /* >>chng 00 nov 28, changed density to 4.9e-9 to reproduce TH85a
                 * when photoionization is turned off. 
                 >>refer        cosmic ray      ionization rate Tielens, A.G.G.M., & Hollenbach, D., 1998, ApJ, 291, 722
                 */
                /* hextra.cryden = 7.07e-9f;*/
                /* this value reproduces the TH cr ionization rate when the factor
                 * of 0.46 is included.  This will directly go onto the h ionization rate
                 * without the factor of 0.46 there.  this is necessary for the more
                 * general case where cr ionization is actually self-consistently determined
                 * from rate hot electrons injected into the plasma */
                /*hextra.cryden = 2.25e-9f;*/
                ASSERT( a > 0. );
                hextra.cryden = hextra.background_density * a;
                hextra.crtemp = 2.6e9f;
        }
        else if( nMatch( "EQUI" , chCard ) )
        {
                /* equipartition cosmic rays, set from B */
                hextra.lg_CR_B_equipartition = true;
                /* this has to be positive for cr's to be on 
                 * it will be reevaluated when B is known */
                hextra.cryden = SMALLFLOAT;
                hextra.crtemp = 2.6e9f;
        }

        else
        {
                /* no keyword found */
                fprintf( ioQQQ, " There must be a keyword on this COSMIC RAY command.\n" );
                fprintf( ioQQQ, " The keywords are DENSITY, RATE, and BACKGROUND.\n" );
                cdEXIT(EXIT_FAILURE);
        }

        /* this is current cosmic ray density divided by background - used in
         * a few chemical reactions */
        hextra.cryden_ov_background = hextra.cryden / hextra.background_density;
        /* >>chng 05 jan 05, 
         * set the cr ionization rate to very rough value, before we have enough
         * information to evaluate it - may be needed in initial guess of H and He ionization*/
        ionbal.CosRayIonRate = hextra.cryden_ov_background * 2.5e-17;

        /* vary option */
        if( optimize.lgVarOn )
        {
                /* will be one parameter */
                optimize.nvarxt[optimize.nparm] = 1;
                strcpy( optimize.chVarFmt[optimize.nparm], "COSMic rays LOG BACKGROUND=%f" );
                /* array index for where to write */
                optimize.nvfpnt[optimize.nparm] = input.nRead;
                /* log of cosmic rays rates relative to background */
                optimize.vparm[0][optimize.nparm] = (realnum)log10(a);
                /* the increment in the first steps away from the original value */
                optimize.vincr[optimize.nparm] = 0.2f;
                ++optimize.nparm;
        }

        return;
}

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