pressure.cpp

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/* This file is part of Cloudy and is copyright (C)1978-2022 by Gary J. Ferland and
 * others.  For conditions of distribution and use see copyright notice in license.txt */
#include "cddefines.h"
#include "pressure.h"
#include "rfield.h"
#include "transition.h"
#include "rt_escprob.h"

t_pressure pressure;

void t_pressure::zero()
{
        DEBUG_ENTRY( "t_pressure::zero()" );
        /* pressure related variables */

        RhoGravity_dark = 0.;
        RhoGravity_self = 0.;
        RhoGravity_external = 0.;
        RhoGravity = 0.;
        IntegRhoGravity = 0.;
        gravity_symmetry = -1;
        self_mass_factor = 1.;

        PresRamCurr = 0.;
        pres_radiation_lines_curr = 0.;
        lgPradCap = false;
        lgPradDen = false;
        lgLineRadPresOn = true;
        /* normally abort when radiation pressure exceeds gas pressure in const pres mod,
         * this is option to keep going, set with NO ABORT on constant pressure command */
        lgRadPresAbortOK = true;
        /* Ditto for whether to stop at sonic point, this gets set to false
         * for some of the dynamics pressure modes (strongd, shock, antishock)*/
        lgSonicPointAbortOK = true;
        /* this flag will say we hit the sonic point */
        lgSonicPoint = false;
        /* True when no physical solution for desired pressure in strong D fronts */
        lgStrongDLimbo = false; 

        RadBetaMax = 0.;
        ipPradMax_nzone = -1;
        PresMax = 0.;

        /* initial and current pressures */
        PresTotlInit = 0.;
        PresTotlCurr = 0.;

}

double PressureRadiationLine( const TransitionProxy &t, realnum DopplerWidth )
{
        DEBUG_ENTRY( "PressureRadiationLine()" );

        /* return zero if below plasma frequency */     
        if( t.EnergyErg() / EN1RYD <= rfield.plsfrq )
                return 0.;

        /* RT_LineWidth gets line width in terms of RT effects */
        double width = RT_LineWidth(t, DopplerWidth);

        double PopOpc = t.Emis().PopOpc()/(*t.Lo()).g();
        /* return zero line radiation PressureReturned if line mases or has
         * zero opacity */
        /* \todo 2 1e-22 is arbtrary but roughly 1/kpc.  Replace with a cloud width if available? */
        if( t.Emis().VoigtLineCen() * PopOpc*t.Emis().opacity()/ DopplerWidth <= 1.e-22 || width<=0. )
                return 0.;

        double PressureReturned = PI8 * HPLANCK / 3. * POW4(t.EnergyWN()) *
                ((*t.Hi()).Pop()/(*t.Hi()).g())/PopOpc * width;

        /* this prevents line radiation PressureReturned from being very large when line 
         * is not optically thick but total opacity at that energy is large 
         * due to overlapping transitions */
        long int ipLineCenter = t.Emis().ipFine() + rfield.ipFineConVelShift;
        if( ipLineCenter > 0 && ipLineCenter < rfield.nfine && rfield.lgOpacityFine &&
                rfield.fine_opac_zone[ipLineCenter] > SMALLFLOAT )
        {
                double FractionThisLine = t.Emis().VoigtLineCen() * t.Emis().PopOpc() * t.Emis().opacity() /
                        DopplerWidth / rfield.fine_opac_zone[ipLineCenter];
                if( FractionThisLine<1e-5 )
                        FractionThisLine = 0.;
                /* fine opacities are only reevaluated one time per zone due
                 * to the expense - PopOpc is for the current solution - but the two
                 * may be out of step by a few percent, due to the variation in
                 * abundance from zone to zone.  This prevents the change
                 * in solution from increasing the radiation pressure.
                 * This correction is mainly an order of magnitude scaler to prevent
                 * optically thin lines from appearing to be optically thick due to
                 * overlapping lines */
                FractionThisLine = MIN2(1., FractionThisLine);
                ASSERT( FractionThisLine >= 0. && FractionThisLine <= 1.0 );
                PressureReturned *= FractionThisLine;
        }

        return PressureReturned;
}