highen.cpp

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/* This file is part of Cloudy and is copyright (C)1978-2013 by Gary J. Ferland and
 * others.  For conditions of distribution and use see copyright notice in license.txt */
/*highen do high energy radiation field - gas interaction, Compton scattering, etc */
#include "cddefines.h"
#include "physconst.h"
#include "trace.h"
#include "heavy.h"
#include "radius.h"
#include "magnetic.h"
#include "hextra.h"
#include "thermal.h"
#include "dense.h"
#include "doppvel.h"
#include "ionbal.h"
#include "rfield.h"
#include "opacity.h"
#include "gammas.h"
#include "highen.h"
#include "pressure.h"

void highen( void )
{
        long int i,
                ion,
                nelem;

        double CosRayDen, 
          crsphi, 
          heatin, 
          sqthot;

        double hin;

        DEBUG_ENTRY( "highen()" );


        /**********************************************************************
         *
         *                                              COMPTON RECOIL IONIZATION
         *
         * bound electron scattering of >2.3 kev photons if neutral
         * lgComptonOn usually t, f if "NO COMPTON EFFECT" command given
         * lgCompRecoil usually t, f if "NO RECOIL IONIZATION" command given 
         *
         **********************************************************************/

        /* lgComptonOn turned false with no compton command,
         * lgCompRecoil - no recoil ionization */
        if( rfield.lgComptonOn && ionbal.lgCompRecoil )
        {
                for( nelem=0; nelem<LIMELM; ++nelem )
                {
                        for( ion=0; ion<nelem+1; ++ion )
                        {
                                ionbal.CompRecoilIonRate[nelem][ion] = 0.;
                                ionbal.CompRecoilHeatRate[nelem][ion] = 0.;
                                if( dense.xIonDense[nelem][ion] > 0. )
                                {
                                        /* recoil ionization starts at 194 Ryd = 2.6 keV */
                                        /* this is the ionization potential of the valence shell */
                                        /* >>chng 02 may 27, lower limit is now 1 beyond actual threshold
                                         * since recoil energy at threshold was very small, sometimes negative */
                                        for( i=ionbal.ipCompRecoil[nelem][ion]; i < rfield.nflux; ++i)
                                        {
                                                double recoil_energy;
                                                crsphi = opac.OpacStack[i-1+opac.iopcom] * rfield.SummedCon[i] *
                                                        /* this is number of electrons in valence shell of this ion */
                                                        ionbal.nCompRecoilElec[nelem-ion];

                                                /* direct hydrogen ionization due to compton scattering, 
                                                 * does not yet include secondaries,
                                                 * last term accounts for number of valence electrons that contribute */
                                                ionbal.CompRecoilIonRate[nelem][ion] += crsphi;

                                                /* recoil energy in Rydbergs
                                                 * heating modified for suprathermal secondaries below; ANU2=ANU**2 */
                                                /* >>chng 02 mar 27, use general formula for recoil energy */
                                                /*energy = 2.66e-5*rfield.anu2[i] - 1.;*/
                                                recoil_energy  = rfield.anu2[i] / 
                                                        ( EN1RYD * ELECTRON_MASS * SPEEDLIGHT * SPEEDLIGHT) * EN1RYD* EN1RYD - 
                                                        Heavy.Valence_IP_Ryd[nelem][ion];

                                                /* heating is in rydbergs because SecIon2PrimaryErg, SecExcitLya2PrimaryErg, HeatEfficPrimary in ryd */
                                                ionbal.CompRecoilHeatRate[nelem][ion] += crsphi*recoil_energy;
                                        }
                                        /* net heating rate, per atom, convert ryd/sec/cm3 to ergs/sec/atom */
                                        ionbal.CompRecoilHeatRate[nelem][ion] *= EN1RYD;

                                        ASSERT( ionbal.CompRecoilHeatRate[nelem][ion] >= 0.);
                                        ASSERT( ionbal.CompRecoilIonRate[nelem][ion] >= 0.);
                                }
                        }
                }
        }
        else
        {
                for( nelem=0; nelem<LIMELM; ++nelem )
                {
                        for( ion=0; ion<nelem+1; ++ion )
                        {
                                ionbal.CompRecoilIonRate[nelem][ion] = 0.;
                                ionbal.CompRecoilHeatRate[nelem][ion] = 0.;
                        }
                }
        }

        /**********************************************************************
         *
         *                          COSMIC RAYS
         *
         * heating and ionization by cosmic rays, other relativistic particles
         * CRYDEN=density (1/CM**3), neutral rate assumes 15ev total
         * energy loss, 13.6 into ionization, 1.4 into heating
         * units erg/sec/cm**3
         * iff not specified, CRTEMP is 2.6E9K
         *
         **********************************************************************/

        if( hextra.cryden > 0. )
        {
                ASSERT( hextra.crtemp > 0. );
                /* this is current cosmic ray density, as determined from original density times
                 * possible dependence on radius */
                if( hextra.lg_CR_B_equipartition )
                {
                        /* >>chng 06 jun 02, add this option
                         *  this is case where cr are in equipartition with magnetic field -
                         * set with COSMIC RAY EQUIPARTITION command */
                        CosRayDen = hextra.background_density * 
                                /* ratio of energy density in current B to typical galactic
                                 * galactic background energy density of 1.8 eV cm-3 is from
                                 *>>refer       cr      background      Webber, W.R. 1998, ApJ, 506, 329 */ 
                                magnetic.energydensity / 
                                (CR_EDEN_GAL_BACK_EV_CMM3/*1.8eV cm-3*/ * EN1EV/*erg eV-1*/ );
                }
                else
                {
                        /* this is usual case, CR density may depend on radius, usually does not */
                        CosRayDen = hextra.cryden*pow(radius.Radius/radius.rinner,(double)hextra.crpowr);
                }

                /* cosmic ray energy density rescaled by ratio to background ion rate and B field */
                hextra.cr_energydensity = CosRayDen/hextra.background_density * 
                        (CR_EDEN_GAL_BACK_EV_CMM3/*1.8eV cm-3*/ * EN1EV/*erg eV-1*/ );

                /* related to current temperature, when thermal */
                sqthot = sqrt(hextra.crtemp);

                /* rate hot electrons heat cold ones, Balbus and McKee 1982
                 * units erg sec^-1 cm^-3,
                 * in sumheat we will multipy this rate by sum of neturals, but for this
                 * term we actually want eden, so mult by eden over sum of neut */
                ionbal.CosRayHeatThermalElectrons = 5.5e-14/sqthot*CosRayDen;

                /* ionization rate; Balbus and McKee */
                ionbal.CosRayIonRate = 1.22e-4/sqthot*
                        log(2.72*pow(hextra.crtemp/1e8,0.097))*CosRayDen;

                /* option for thermal CRs, first is the usual (and default) relativistic case */
                if( hextra.crtemp > 2e9 )
                {
                        /* usual circumstance; relativistic cosmic rays, 
                         * cosmic ray ionization rate s-1 cm-3; ext rel limit */
                        ionbal.CosRayIonRate *= 3.;

                }
                else
                {
                        /*  option for thermal cosmic rays */
                        ionbal.CosRayIonRate *= 10.;
                }
                /* >>chng 04 jan 27, from 0.093 to 2.574 as per following */
                /* cr heating from Table 1 of
                 *>>refer       cr      heating Wolfire et al.1995, ApJ, 443, 152
                 * For every ionization due to cosmic rays, ~35eV of heat is added 
                 * to the system.  This manifests itself in the ionbal.CosRayHeatNeutralParticles term
                 * by the 2.574*EN1RYD term, which is just the energy in ergs in 35 eV.
                 * Change made by Nick Abel and Gargi Shaw, 04 Jan 27.   In heatsum 
                 * we  multiply by the number of secondaries that occur */
                ionbal.CosRayHeatNeutralParticles = ionbal.CosRayIonRate*2.574*EN1RYD;

                if( trace.lgTrace )
                {
                        fprintf( ioQQQ, "     highen: cosmic ray density;%10.2e CRion rate;%10.2e CR heat rate=;%10.2e CRtemp;%10.2e\n", 
                          CosRayDen, ionbal.CosRayIonRate, ionbal.CosRayHeatNeutralParticles, hextra.crtemp );
                }
        }
        else
        {
                ionbal.CosRayIonRate = 0.;
                ionbal.CosRayHeatNeutralParticles = 0.;
        }
        /* >>chng 06 may 23, Penning ionization
        ionbal.CosRayIonRate += 1e-9 * 
                iso_sp[ipHE_LIKE][ipHELIUM].st[ipHe2s3S].Pop; */

        /*fprintf(ioQQQ,"DEBUG cr %.2f %.3e %.3e %.3e\n",
                fnzone,
                hextra.cryden ,
                ionbal.CosRayIonRate ,
                ionbal.CosRayHeatNeutralParticles );*/

        /**********************************************************************
         *
         * add on extra heating due to turbulence, goes into [1] of [x][0][11][0]
         *
         **********************************************************************/

        /* TurbHeat added with hextra command, DispScale added with turbulence dissipative */
        if( (hextra.TurbHeat+DoppVel.DispScale) != 0. )
        {
                /* turbulent heating only goes into the low-energy heat of this element */
                /* >>>>chng 00 apr 28, functional form of radius dependence had bee turrad/depth
                 * and so went to infinity at the illuminated face.  Changed to current form as
                 * per Ivan Hubeny comment */
                if( hextra.lgHextraDepth )
                {
                        /* if turrad is >0 then vary heating with depth */
                        ionbal.ExtraHeatRate = 
                                hextra.TurbHeat*sexp(radius.depth /hextra.turrad);

                        /* >>chng 00 aug 16, added option for heating from back side */
                        if( hextra.turback != 0. )
                        {
                                ionbal.ExtraHeatRate += 
                                        hextra.TurbHeat*sexp((hextra.turback - radius.depth) /hextra.turrad);
                        }
                }
                else if( hextra.lgHextraDensity )
                {
                        /* depends on density */
                        ionbal.ExtraHeatRate = 
                                hextra.TurbHeat*dense.gas_phase[ipHYDROGEN]/hextra.HextraScaleDensity;
                }
                else if( hextra.lgHextraSS )
                {
                        /* with SS disk model */
                        ionbal.ExtraHeatRate = 
                          hextra.HextraSSalpha*pressure.PresGasCurr*pow(hextra.HextraSS_M*GRAV_CONST*
                                        pow((double)hextra.HextraSSradius,-3.0),0.5);
                }
                /* this is turbulence dissipate command */
                else if( DoppVel.DispScale > 0. )
                {
                        double turb = DoppVel.TurbVel * sexp( radius.depth / DoppVel.DispScale );
                        /* if turrad is >0 then vary heating with depth */
                        /* >>chng 01 may 10, add extra factor of length over 1e13 cm */
                        ionbal.ExtraHeatRate = 3.45e-28 / 2.82824 * turb * turb * turb *
                                        ( dense.gas_phase[ipHYDROGEN] / 1e10 ) / (DoppVel.DispScale/1e13);
                }
                else
                {
                        /* constant extra heating */
                        ionbal.ExtraHeatRate = hextra.TurbHeat;
                }
        }

        else
        {
                ionbal.ExtraHeatRate = 0.;
        }

        /**********************************************************************
         *
         * option to add on fast neutron heating, goes into [0] & [2] of [x][0][11][0]
         *
         **********************************************************************/
        if( hextra.lgNeutrnHeatOn )
        {
                /* hextra.totneu is energy flux erg cm-2 s-1
                 * CrsSecNeutron is 4E-26 cm^-2, cross sec for stopping rel neutrons
                 * this is heating erg s-1 due to fast neutrons, assumed to secondary ionize */
                /* neutrons assumed to only secondary ionize */
                ionbal.xNeutronHeatRate = hextra.totneu*hextra.CrsSecNeutron;
        }
        else
        {
                ionbal.xNeutronHeatRate = 0.;
        }


        /**********************************************************************
         *
         * pair production in elec field of nucleus 
         *
         **********************************************************************/
        t_phoHeat photoHeat;
        ionbal.PairProducPhotoRate[0] = GammaK(opac.ippr,rfield.nflux,opac.ioppr,1.,&photoHeat);
        ionbal.PairProducPhotoRate[1] = photoHeat.HeatLowEnr;
        ionbal.PairProducPhotoRate[2] = photoHeat.HeatHiEnr;

        /**********************************************************************
         *
         * Compton energy exchange 
         *
         **********************************************************************/
        rfield.cmcool = 0.;
        rfield.cmheat = 0.;
        heatin = 0.;
        /* lgComptonOn usually t, turns off Compton */
        if( rfield.lgComptonOn )
        {
                for( i=0; i < rfield.nflux; i++ )
                {

                        /* Compton cooling
                         * CSIGC is Tarter expression times ANU(I)*3.858E-25
                         * 6.338E-6 is k in inf mass Rydbergs, still needs factor of TE */
                        rfield.comup[i] = (double)(rfield.flux[0][i]+rfield.ConInterOut[i]+
                          rfield.outlin[0][i]+ rfield.outlin_noplot[i])*rfield.csigc[i]*(dense.eden*4.e0*
                          6.338e-6*1e-15);

                        rfield.cmcool += rfield.comup[i];

                        /* Compton heating 
                         * CSIGH is Tarter expression times ANU(I)**2 * 3.858E-25
                         * CMHEAT is just spontaneous, HEATIN is just induced */
                        rfield.comdn[i] = (double)(rfield.flux[0][i]+rfield.ConInterOut[i]+
                           rfield.outlin[0][i]+ rfield.outlin_noplot[i])*rfield.csigh[i]*dense.eden*1e-15;

                        /* induced Compton heating */
                        hin = (double)(rfield.flux[0][i]+rfield.ConInterOut[i]+rfield.outlin[0][i]+rfield.outlin_noplot[i])*
                          rfield.csigh[i]*rfield.OccNumbIncidCont[i]*dense.eden*1e-15;
                        rfield.comdn[i] += hin;
                        heatin += hin;

                        /* following is total compton heating */
                        rfield.cmheat += rfield.comdn[i];
                }

                /* remember how important induced compton heating is */
                if( rfield.cmheat > 0. )
                {
                        rfield.cinrat = MAX2(rfield.cinrat,heatin/rfield.cmheat);
                }

                if( trace.lgTrace && trace.lgComBug )
                {
                        fprintf( ioQQQ, "     HIGHEN: COOL num=%8.2e HEAT num=%8.2e\n", 
                          rfield.cmcool, rfield.cmheat );
                }
        }

        /* save compton heating rate into main heating save array, 
         * no secondary ionizations from compton heating cooling */
        thermal.heating[0][19] = rfield.cmheat;

        if( trace.lgTrace && trace.lgComBug )
        {
                fprintf( ioQQQ, 
                        "     HIGHEN finds heating fracs= frac(compt)=%10.2e "
                        " f(pair)%10.2e totHeat=%10.2e\n", 
                  thermal.heating[0][19]/thermal.htot, 
                  thermal.heating[0][21]/thermal.htot,
                  thermal.htot  );
        }
        return;
}