Ztrackp.h

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!           Parameters used for Tracking.
!   (-> --------------------------------------------

          integer  Eabsorb(2)   !2  If (1)=0, no call to chookEabsorb or chookEabsorb2 is made.
          !  (2) is used to indicate later at which the user want to
         !  energy sum of particles falling on it.
             !  If (1) is non zero, when a charged particle makes energy loss to Air, chookEabsorb is 
             !  always called. When a particle dies (i.e, it K.E becomes < Emin), chookEabsorb2
             !  may be called dedpending on the particle and Eabsorb bit. (LSB is bit 1).
             !  calling cond (See Ztrackv.h, BitPhoton etc).
             !  bit 2  and photon.  bit 3 and e-/e+. bit 4 proton. bit 5 neutron
             !  bit 6 anti-N.  bit 7 decayable ptcl, bit8 others 
             !  bit 1 is for photoelectric effect but is not used in Air.

         logical  ExactThick   !2  If T, a given length is converted into thickness with best accuracy even for very 
                              !  inclined trajectory by using numerical integration.
        logical IncMuonPolari  !1  if T, consider muon polarization
        integer HowPhotoP      !2  if 0--> no photo hadron prod.
          !      1--> Sofia at all E
          !      2--> Exp. data < 2.5 GeV ; Sofia > 2.5GeV
          !      3--> Sofia < 2.5GeV;  (rho, omega, phi) or pi0 or pi+/- at current model
         !      4--> Exp. data < 2.5GeV   //
         integer  PhitsXs !2 when phits is used, specify the Xsection to be used.
                !  D=0.   Use cosmos xsection               
                !  bit 1--> for p,n use phits xs (last bit is bit 1) (btest(..,0)-->T
                !  bit 2--> for heavy, use phits xs.        
                !  (phits xs seems to be too large)
 
     integer JamXs        !2      0--> use inelastic channel only with Cosmos cross-section
                              !      1--> use total cross-section  with Cosmos cross-section
         integer AAXsec  !2  =1 AA cosmos xsection is normalized to Shen's one at 5GeV/n if
            !     E/n > 5 GeV and used; E/n< 5 GeV, Shen's xs is used
            !  =0 AA Shen's xsection is normalzied to cosmos Xsection at 
            ! 5GeV if E/n < 5 GeV and used; E/n>5 cosmos xs is used
         integer JamFragment  !2     0--> as original Jam, the spectator breaks into nucleons
            !      1--> spectator goes into nucleons, some light heavy ions and heavy remnants
           !           the method is simple but not so bad.
        logical Freec          !1  if F, the first interaction point is forced to be the injection point else
                               !   the interaction poin is randomly sampled.
         integer OneDim        !1  If 0, 3 dimensional simulation. if $\ge$1, one
                               !  dimensional simulation is performed.  \newline
                               !  1: onedim without use of table. \newline
                               !  2: table is used for thickness $ \leftrightarrow$ length conversion. if cos $<$ .5 \newline
                               !  3: table is always used for any angle.
                               !  ( for height $>$ 30 km, table is not used in any case). 
        real*8  LamorDiv       !2  In the geomagnetic field, a charged particle can travel almost streight 
                               !  in (Lamor Radius)/LamorDiv.  Default is 5. For AMS like tracking 20 may be needed.
         real*8  Truncc         !2 coeff. for truncating path.
         real*8  Truncn         !2 coeff. for truncating path.
         real*8  Truncx         !2 coeff. for truncating path.
         real*8  KEminObs(8)    !1  The min kinetic energy of particles for observation.
          !  KEminObs(i): i=1 is for g, 2 e, 3 mu, 4 pi, 5 K, 6 N, 7 Neu, 8 other
         !  default is 2*500keV,7*10MeV. i=2 is foreced to be the same as i=1.
          !  Normally the user may define only i=1.
         real*8  KEminObs2(8)      !2  Don't touch this. skeleton/flesh use.
         real*8  RatioToE0      !2 In the A.S generation,  hadronic interactions are followed down to at
                               !  least  RatioToE0 * E0/nucleon energy.
        real*8  WaitRatio      !1  Wait A.S generation until the electron energy, Ee, becomes $<$ WaitRatio* E0. 
                               !   This many be 1.0 for hadron origin case. But for gamma/electron primary, 
                               !   this should be as low as 0.01 to enjoy full fluctuation.
        integer EndLevel !2 Used for skeleton/flesh-out job. In a normal job, system default value 0 is reset by
            ! the system to be the max number of observation levels. (=NoOfSites).  Its real use is in such a
            ! skeleton/flesh-out job that one first follows the particles up to some high depth and later chooses
            ! events and flesh them out to deeper depths. In such a skeleton-making job, the user must give the
            ! depth list which is used flesh-out job, too.  In the skeleton job, particle tracking is terminated
            ! at the level specified by EndLevel.  In such a flesh-out job, the user must give a larger value 
            ! or 0 to EndLevel 
        integer EndLevel2 !2  Don't worry. This  is system use.
         integer Trace   !1  Flag for trace information output.\newline
            !   0 $\rightarrow$ no trace information is output.\newline
            !  $<$10$\rightarrow$ x, y, z in the primary system(say, 1)\newline
            !  $<$20 $\rightarrow$ x, y, in the primary sys. z in kg/m$^2$.(say,11)\newline
            !  $<$30 $\rightarrow$ x, y, z in the detector system\newline
            !  $<$40 $\rightarrow$ x, y, in the detector system. z in kg/m2\newline 
            !  $<$50 $\rightarrow$ x, y, z in 'xyz' system.\newline
            !  $<$60 $\rightarrow$ x,y, in 'xyz' and z in kg/m2\newline
            !  61-100 $\rightarrow$  for Cherenkov observation. For Coord system,  subtract 60.\newline
            !   if the value is even,  binary output is made on TraceDev.\newline
            !   if the last digit is 1 or 2, trace is always taken. if the last digit is 3 or 4, trace is taken
            !   only if the particle is located below the heighest observation depeth. 
            !  $>$ 101  $\rightarrow$ subtract 100 and apply the above, but chookTrace or chookCeren are used.\newline
            !  Primary system:  Origin is the deepest detector.  Z-axis is the primary direction. 
            !                   X-axis is Z x Vertical axis.  X-Y plane is orthogonal to the primary.\newline
            !  Detector system: origin is the deepest detector. Z-axis is the vertical one.  X-axis is 
            !                   directed to the magnetic east.  X-Y plane is horizontal.\newline
            !  z in kg/m$^2$ :     Vertical depth in kg/m$^2$  above the  deepest detector to the particle.
         integer TraceDev      !2  Logical dev \# for TraceDir/trace1,2,.... 
        character*70  TraceDir !1 Directory.  Default Trace information is put TraceDir/trace1, 2,..
                               ! for event 1, 2, ... The directory should exist.  Default is ' ' and in this case
                               ! /tmp/YourLoginName/ is employed. The last "/" should not be given.
                               ! *** NOTE that default Cherenkov output is made only using TraceDev,
                               !    TraceDir is not used.  You have to open the disk file at chookbgRun
                               !    It can by binary or ascii file depending on Trace value.
         logical ThinSampling  !1  if F, thinsampling is not tried. if T, alla Hillas thinning. Don't use with
                              !    the  skeleton/flesh method 
        real*8  EthinRatio(4) !2  if ThinsSamplig == T, thin sampling is performed if the energy of a particle is
                              !  between (EthinRatio(2)$\sim$EthinRatio(1))* PrimaryEnergy(/nucleon)
                              !   (=Ethin(2)$sim$Ethin(1)) ( EtinRatio(1)$>$ 0).
                              !  If EthinRatio(1) $<$ 0, Ethin will be |EthinRatio| (GeV). 
                              !  (1),(2) is for e/g. (3),(4) is for mu/hadron.  if(3)(4) are not given, 
                              !  (3)=(1)/10 and (4)=(2)/10 are used.
        logical TimeStructure !1  If T,  time information is computed
         integer HowGeomag     !2  if 1, no magnetic field until first coll. \newline
                              !      2, mag.f always exists. If Reverse not=0, use this. \newline
                              !     11, same as 1 but mag.f is const. \newline
                              !     12, same as 2 but mag.f is const. \newline
                              !     21, same as 1 but mag.f is const. \newline
                              !     22, same as 2 but mag.f is const.  \newline
                              !     31, same as 1 but mag.f is dependent on the position.  \newline
                              !  const value is the one at deepest observation plane. for 11,12  or should be given by
                              !  MagN, MagE, MagD for 21, 22. For normal applications,  11 is good.
                              !  If no magnetic field is applied, energy loss by dE/dx is considered.(bef.4.92,
                              !  and aft. 5.14)
        real*8  MagN          !2 See HowGeomag (in Tesla)
         real*8  MagE          !2 See HowGeomag (in Tesla)
        real*8  MagD          !2 See HowGeomag (in Tesla)

        real*8  MagChgDist    !2 Distance where mag. can be seen  as const.(m) at sea level
        integer UseRungeKutta !2 How to calculate deflection by the geomagnetic field. Let L be the distance
                              !   the  particle travels. \newline
                              ! 0$\rightarrow$Don't use RungeKutta method. Use the solution assuming the constant B, which
                              !     is exact if B is const.  Since the particle path is made  short, this is
                              !     enough for normal cases where particles are inside the atmosphere.(default) \newline
                              !     In every case below, if the particle height is $<$ 30km  
                              !    (= cheight in ccomPathEnd.f), the same method as 0 is used. \newline
                              ! 1$\rightarrow$ Use the Euler method.  Time needed is 20\% more than the 0 case.
                              !      As B, use the value at L/2 point obtained by using the current direction. \newline
                              ! 2$\rightarrow$ mixture of 1 and Runge-Kutta-Gill method. If gradient of B is large, RKG is
                              !      employed. This needs $\sim$4 times more cpu time than case of 1 when making a
                              !      cutoff table.  The step size of RKG is $\sim$1/10 of the Lamore radius. \newline
                              ! 3$\rightarrow$ The same as 2 but use the Runge-Kutta-Fehlberg method instead of RKG.
                              !      Step size is automattically adjusted ($\sim$1/20 $\sim$1/30 of Lamor radius) \newline
                              ! 4$\rightarrow$ As a middle point, use the point obtained by assuming the constant B at
                              !      initial point. If grad B is still large, use RKG. \newline
                              ! 5$\rightarrow$ The same as 4 but us RKF instead of RKG. \newline
                              ! 6$\rightarrow$ Use always RKG \newline
                              ! 7$\rightarrow$ Use always RKF.  This takes very long time.(50 times of 0). \newline
         real*8  BorderHeightH !2 If a particle goes higher than this, discard it.  This should be larger than 
                              !  HeightOfInj or 0.  
                              !  If 0, it is adjusted to be the same as HeightOfInj. NOTE: For upgoin primary cases, you have
                              !  to set this one explicitly. 
         real*8  BorderHeightL !2 If a particle reaches this hight, call observation routine. No further tracking is done. 
                              !  This is for neutrino observation.  See ObsPlane.
        real*8  BackAngLimit  !2 If the cosine of the angle between a particle and the primary becomes smaller than
                              !  this value, the particle is discarded. See also BorderHeighH. If you give a value 
                              !  less than -1.0, such rejection will never happen.   Default is -1.0
         character*16 Generate !1 specify what should be generated \newline
                              !   1)  Electro-magnetic cascade(em), \newline
                              !   2)  one dimensional  hybrid AS(as/qas) and/or \newline
                              !   3)  AS Lateral distribution(lat). \newline
                              !    If Generate= ' ', hadronic cascade shower is generated. \newline
                              !  For example, you may give as follows: \newline
                              !    Generate='em,as' or 'em/as' (order/case/separator insensitive) is to  generate EM-cascade and AS. \newline
                              !    Generate='as' will  generate AS with some  adequate EM cascade (EM cascade is automatically generated
                              !    so that hybrid A.S can be observed, but the minimum energy in EM cascade is independent of KEminObs). \newline
                              !   If 'qas' is given, quick generation of AS for heavy primaries is tried. See  chookASbyH.f 

        character*16 Generate2 !2  don't touch this.  for skeleton/flesh use.

         integer MagBrem       !2 If 0, no magnetic bremsstrahlung is considered. \newline
                              ! if 1 and Ee $>$ MagBremEmin, energy loss due to magnetic brems is considered \newline
                              ! if 2 and Ee $>$ MagBremEmin, real sampling of gamma is performed. \newline
                              ! (note, actually upsilon is referred further).
                              ! if generate='as' with really high energy primaries, WaitRatio
                              ! must be made small so that WaitRatio*E0 $\sim$ MagBremEmin 
        integer MagPair       !2 If 0, no magnetic pair creation is considered. \newline
                              !  if 1 and Eg > MagPairEmin, real sampling is tried.
                              ! (note, actually upsilon is referred further).  To see these magnetic effects,
                              !  HowGeoMag=2 and HightOfInj $\sim$ 5000 km are desirable.

        logical LpmEffect     !1 If t, the LPM effect is  considered when Ee $>$ LpmBremEmin for electrons and
                              !        Eg $>$ LpmPairEmin for gamma rays.

        real*8  MagBremEmin   !2  E $>$ this, magnetic bremsstrahlung by electrons may be considered. However, if
                              !   MagBrem = 0, not considered at all \newline
                              !   MagBrem = 1, total energy loss due to brems is considered. \newline
                              !   MagBrem = 2, gamma energy is sampled actually. \newline
                              !   If upsilon (Ee/m * B/Bcr) is small, the effective treatment will be
                              !   the same as MagBrem = 0 case.
        real*8  MagPairEmin   !2  E $>$ this, magnetic pair creation by gamma may be considered. However, if
                              !   MagPair = 0, not considered at all. \newline
                              !   MagPair = 1, pair creation is sampled.  \newline
                              !   However, again, actual occurrence will be dependent on the angle between
                              !   B and photon direction.
        real*8  UpsilonMin    !2  Magnetic bremsstralhung is considered only if upsilon $>$ UpsilonMin.
        real*8  LpmBremEmin   !2  The LPM effect is taken into account for bremsstrahlung when LpmEffect is .true. 
                              !   and the electron energy is higher than this.
        real*8  LpmPairEmin   !2  The LPM effect is taken into account for pair creation when LpmEffect is .true.
                              !    and the gamma energy is higher than this.
        real*8  StepControl   !2   When  observation depth step becomes small,
                              ! high energy partciles may go that step without
                              ! suffering from scattering and this could lead to
                              ! under estimation of lateral spread (We don't impose
                          ! scattering when a particle cross the observation depth
                              ! by technical reason.) StepControl
                              ! is used to make the maximum step size of particles
                              ! to be at most (depth step)/StepControl.  Default is 5.
        integer Reverse       !2  0$\rightarrow$ Normal tracking. \newline
                              !   1$\rightarrow$ incident is tracked to a direction opposite to the given one.
                              !       the incident is charge-conjugated.
                              !       All interactions are ignored. (Use when to make cut-off table or to see
                              !       a given particle (say, observed anti proton) can go out of Earth. \newline
                              !   2$\rightarrow$ same as 1 but energy gain (not loss) is taken into account
                              !   TimeStructure should be T if Reverse != 0.  See BackAnglLimit.

        real*8 PathLimit      !2  If the sum of (path/beta) of a particle  exceeds this, it is judged as dead.
                              !   (to avoid infinite cyclotron loop).  However, for normal applications,
                              !   this will not be effective because of BackAnglLimit. See Reverse.
                              !   TimeStructure should be T if Reverse != 0 and PathLimit is to be effective.

       integer MuNI           !2 0$\rightarrow$ nuclear interaction of muon is completely neglected \newline
                              !  1$\rightarrow$ energy loss by n.i is subsumed in dE/dx of muons as a continuous energy loss.  Let v=
                              !     Etransfer/Emu,  the loss here is Int(vc:vmax) of (Emu vdsigma/dv).  (vc $\sim$0, vmax$\sim$1). \newline
                              !  2$\rightarrow$ (Default value). similar to 1 but as the continuous loss only v $<$ vmin=10$^{-3}$ of
                              !     fractional muon energy is subsumed (Int(vc: vmin) of (Emu vdsigma/dv)).  The portion
                              !     of loss by v$>$vmin is treated as a stocastic  process.  However, the product from the
                              !     n.i itself is neglected \newline
                              !  3$\rightarrow$ the same as 2, but the n.i is explicitly included to produce a number of particles.  
                              !     The n.i is treated as a photo-nucleus interaction.
      integer MuBr            !2  parameter similar to MuNI but for bremsstrahlung by muons.
       integer MuPr           !2  parameter similar to MuNI but for pair creation by muons.

       character(len=2):: ASRforDPM  !  D='m'
               ! "no"  ; don't try to restore Pt asymmetry (
               !         original dpm. some asymmetry for heavy
               !         remnant side.
               ! "r"   ; randomize Pt of mesons for Pz< 2GeV
               !         in target rest frame and proj. rest frame
               ! "r1"  ; do the same only for target rest frame
               ! "m"   ; x <= -x  sign change with prob. of 1/2
               !          for all particles. 
               !However, If proj = p,pi.. and Target A<6, no ASR
               !         If proj A<6 and target A<6, also no ASR
!    <-)    ----------------------------------------------

         common /cZtracp/ Truncc, Truncn, Truncx, 
     *  KEminObs, KEminObs2, RatioToE0, PathLimit,
     *  WaitRatio,  EthinRatio, BackAngLimit, LamorDiv,
     *  BorderHeightH,  MagN, MagE, MagD, MagChgDist,
     *  BorderHeightL,  MuNI, MuBr, MuPr,
     *  MagBremEmin, MagPairEmin, UpsilonMin, LpmBremEmin, 
     *  LpmPairEmin, UseRungeKutta, StepControl,
     *  ThinSampling, TimeStructure, HowGeomag,
     *  Trace, TraceDev,  ExactThick, OneDim, Reverse,
     *  Freec,  IncMuonPolari, MagBrem, MagPair, LpmEffect,
     *  EndLevel, EndLevel2, Eabsorb, HowPhotoP, PhitsXS,
     *  JamXs, AAXsec, JamFragment
 
        common /cZtrackpc/
     *  Generate, Generate2, TraceDir, ASRforDPM