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Functions | |
| ! 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 |
| ! Parameters used for hadronic cascade shower is generated newline ! For you may give as as or em | as (order/case/separator insensitive) is to generate EM-cascade and AS. \newline ! Generate |
| ! Parameters used for hadronic cascade shower is generated newline ! For you may give as as or em quick generation of AS for heavy primaries is tried See chookASbyH f character *Generate2 don t touch this for skeleton flesh use integer MagBrem no magnetic bremsstrahlung is considered newline ! if and Ee energy loss due to magnetic brems is considered newline ! if and Ee real sampling of gamma is performed | newline (note, actually upsilon is referred further). ! if generate |
| ! Parameters used for hadronic cascade shower is generated newline ! For you may give as as or em quick generation of AS for heavy primaries is tried See chookASbyH f character *Generate2 don t touch this for skeleton flesh use integer MagBrem no magnetic bremsstrahlung is considered newline ! if and Ee energy loss due to magnetic brems is considered newline ! if and Ee real sampling of gamma is performed WaitRatio ! must be made small so that WaitRatio *E0 sim MagBremEmin integer MagPair no magnetic pair creation is considered newline ! if and Eg real sampling is | tried (note, actually upsilon is referred further). To see these magnetic effects |
| ! Parameters used for hadronic cascade shower is generated newline ! For you may give as as or em quick generation of AS for heavy primaries is tried See chookASbyH f character *Generate2 don t touch this for skeleton flesh use integer MagBrem no magnetic bremsstrahlung is considered newline ! if and Ee energy loss due to magnetic brems is considered newline ! if and Ee real sampling of gamma is performed WaitRatio ! must be made small so that WaitRatio *E0 sim MagBremEmin integer MagPair no magnetic pair creation is considered newline ! if and Eg real sampling is the LPM effect is considered when Ee LpmBremEmin for electrons and ! Eg LpmPairEmin for gamma rays real *MagBremEmin E magnetic bremsstrahlung by electrons may be considered if not considered at all newline total energy loss due to brems is considered newline gamma energy is sampled actually newline ! If | upsilon (Ee/m *B/Bcr) is small |
Variables | |
| ! Parameters used for hadronic cascade shower is generated newline ! For | example |
| ! Parameters used for hadronic cascade shower is generated newline ! For you may give as | follows |
| ! Parameters used for hadronic cascade shower is generated newline ! For you may give as as or em quick generation of AS for heavy primaries is tried See chookASbyH f character *Generate2 don t touch this for skeleton flesh use integer MagBrem | If |
| ! Parameters used for hadronic cascade shower is generated newline ! For you may give as as or em quick generation of AS for heavy primaries is tried See chookASbyH f character *Generate2 don t touch this for skeleton flesh use integer MagBrem no magnetic bremsstrahlung is considered newline ! if and Ee | MagBremEmin |
| ! Parameters used for hadronic cascade shower is generated newline ! For you may give as as or em quick generation of AS for heavy primaries is tried See chookASbyH f character *Generate2 don t touch this for skeleton flesh use integer MagBrem no magnetic bremsstrahlung is considered newline ! if and Ee energy loss due to magnetic brems is considered newline ! if and Ee real sampling of gamma is performed WaitRatio ! must be made small so that WaitRatio *E0 sim MagBremEmin integer MagPair no magnetic pair creation is considered newline ! if and Eg | MagPairEmin |
| ! Parameters used for hadronic cascade shower is generated newline ! For you may give as as or em quick generation of AS for heavy primaries is tried See chookASbyH f character *Generate2 don t touch this for skeleton flesh use integer MagBrem no magnetic bremsstrahlung is considered newline ! if and Ee energy loss due to magnetic brems is considered newline ! if and Ee real sampling of gamma is performed WaitRatio ! must be made small so that WaitRatio *E0 sim MagBremEmin integer MagPair no magnetic pair creation is considered newline ! if and Eg real sampling is | ! HowGeoMag |
| ! Parameters used for hadronic cascade shower is generated newline ! For you may give as as or em quick generation of AS for heavy primaries is tried See chookASbyH f character *Generate2 don t touch this for skeleton flesh use integer MagBrem no magnetic bremsstrahlung is considered newline ! if and Ee energy loss due to magnetic brems is considered newline ! if and Ee real sampling of gamma is performed WaitRatio ! must be made small so that WaitRatio *E0 sim MagBremEmin integer MagPair no magnetic pair creation is considered newline ! if and Eg real sampling is the LPM effect is considered when Ee LpmBremEmin for electrons and ! Eg LpmPairEmin for gamma rays real *MagBremEmin E | this |
| ! Parameters used for hadronic cascade shower is generated newline ! For you may give as as or em quick generation of AS for heavy primaries is tried See chookASbyH f character *Generate2 don t touch this for skeleton flesh use integer MagBrem no magnetic bremsstrahlung is considered newline ! if and Ee energy loss due to magnetic brems is considered newline ! if and Ee real sampling of gamma is performed WaitRatio ! must be made small so that WaitRatio *E0 sim MagBremEmin integer MagPair no magnetic pair creation is considered newline ! if and Eg real sampling is the LPM effect is considered when Ee LpmBremEmin for electrons and ! Eg LpmPairEmin for gamma rays real *MagBremEmin E magnetic bremsstrahlung by electrons may be considered | However |
| ! Parameters used for hadronic cascade shower is generated newline ! For you may give as as or em quick generation of AS for heavy primaries is tried See chookASbyH f character *Generate2 don t touch this for skeleton flesh use integer MagBrem no magnetic bremsstrahlung is considered newline ! if and Ee energy loss due to magnetic brems is considered newline ! if and Ee real sampling of gamma is performed WaitRatio ! must be made small so that WaitRatio *E0 sim MagBremEmin integer MagPair no magnetic pair creation is considered newline ! if and Eg real sampling is the LPM effect is considered when Ee LpmBremEmin for electrons and ! Eg LpmPairEmin for gamma rays real *MagBremEmin E magnetic bremsstrahlung by electrons may be considered if | ! MagBrem = 0 |
Function Documentation
◆ as()
◆ newline()
| ! Parameters used for hadronic cascade shower is generated newline ! For you may give as as or em quick generation of AS for heavy primaries is tried See chookASbyH f character* Generate2 don t touch this for skeleton flesh use integer MagBrem no magnetic bremsstrahlung is considered newline ! if and Ee energy loss due to magnetic brems is considered newline ! if and Ee real sampling of gamma is performed newline | ( | note | , |
| actually upsilon is referred | further | ||
| ) |
◆ Tracking()
| ! Parameters used for Tracking | ( | -> -------------------------------------------- integer | Eabsorb2) !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 | diesi.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 | xslast 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 | ||
| ) |
◆ tried()
| ! Parameters used for hadronic cascade shower is generated newline ! For you may give as as or em quick generation of AS for heavy primaries is tried See chookASbyH f character* Generate2 don t touch this for skeleton flesh use integer MagBrem no magnetic bremsstrahlung is considered newline ! if and Ee energy loss due to magnetic brems is considered newline ! if and Ee real sampling of gamma is performed WaitRatio ! must be made small so that WaitRatio* E0 sim MagBremEmin integer MagPair no magnetic pair creation is considered newline ! if and Eg real sampling is tried | ( | note | , |
| actually upsilon is referred | further | ||
| ) |
◆ upsilon()
| ! Parameters used for hadronic cascade shower is generated newline ! For you may give as as or em quick generation of AS for heavy primaries is tried See chookASbyH f character* Generate2 don t touch this for skeleton flesh use integer MagBrem no magnetic bremsstrahlung is considered newline ! if and Ee energy loss due to magnetic brems is considered newline ! if and Ee real sampling of gamma is performed WaitRatio ! must be made small so that WaitRatio* E0 sim MagBremEmin integer MagPair no magnetic pair creation is considered newline ! if and Eg real sampling is the LPM effect is considered when Ee LpmBremEmin for electrons and ! Eg LpmPairEmin for gamma rays real* MagBremEmin E magnetic bremsstrahlung by electrons may be considered if not considered at all newline total energy loss due to brems is considered newline gamma energy is sampled actually newline ! If upsilon | ( | Ee/m *B/ | Bcr | ) |
Referenced by cmbrem(), cputenergyloss(), and csampeintl().
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Variable Documentation
◆ ! HowGeoMag
| ! Parameters used for hadronic cascade shower is generated newline ! For you may give as as or em quick generation of AS for heavy primaries is tried See chookASbyH f character* Generate2 don t touch this for skeleton flesh use integer MagBrem no magnetic bremsstrahlung is considered newline ! if and Ee energy loss due to magnetic brems is considered newline ! if and Ee real sampling of gamma is performed WaitRatio ! must be made small so that WaitRatio* E0 sim MagBremEmin integer MagPair no magnetic pair creation is considered newline ! if and Eg real sampling is ! HowGeoMag |
Initial value:
=2 and HightOfInj $\sim$ 5000 km are desirable.
! This namelist data is frequently used ! Some of them should be given mandatory namelist Param LpmEffect
Definition: Znamelist1.h:5
! Parameters used for hadronic cascade shower is generated newline ! For you may give as as or em quick generation of AS for heavy primaries is tried See chookASbyH f character *Generate2 don t touch this for skeleton flesh use integer MagBrem If
Definition: Ztrackp.h:160
◆ ! MagBrem
| ! Parameters used for hadronic cascade shower is generated newline ! For you may give as as or em quick generation of AS for heavy primaries is tried See chookASbyH f character *Generate2 don t touch this for skeleton flesh use integer MagBrem no magnetic bremsstrahlung is considered newline ! if and Ee energy loss due to magnetic brems is considered newline ! if and Ee real sampling of gamma is performed WaitRatio ! must be made small so that WaitRatio *E0 sim MagBremEmin integer MagPair no magnetic pair creation is considered newline ! if and Eg real sampling is the LPM effect is considered when Ee LpmBremEmin for electrons and ! Eg LpmPairEmin for gamma rays real *MagBremEmin E magnetic bremsstrahlung by electrons may be considered if not considered at all newline total energy loss due to brems is considered newline ! MagBrem = 0 |
◆ example
◆ follows
◆ However
| ! Parameters used for hadronic cascade shower is generated newline ! For you may give as as or em quick generation of AS for heavy primaries is tried See chookASbyH f character* Generate2 don t touch this for skeleton flesh use integer MagBrem no magnetic bremsstrahlung is considered newline ! if and Ee energy loss due to magnetic brems is considered newline ! if and Ee real sampling of gamma is performed WaitRatio ! must be made small so that WaitRatio* E0 sim MagBremEmin integer MagPair no magnetic pair creation is considered newline ! if and Eg real sampling is the LPM effect is considered when Ee LpmBremEmin for electrons and ! Eg LpmPairEmin for gamma rays real* MagBremEmin E magnetic bremsstrahlung by electrons may be considered However |
◆ If
| ! Parameters used for hadronic cascade shower is generated newline ! For you may give as as or em quick generation of AS for heavy primaries is tried See chookASbyH f character* Generate2 don t touch this for skeleton flesh use integer MagBrem no magnetic bremsstrahlung is considered newline ! if and Ee energy loss due to magnetic brems is considered newline ! if and Ee real sampling of gamma is performed WaitRatio ! must be made small so that WaitRatio* E0 sim MagBremEmin integer MagPair If |
◆ MagBremEmin
| ! Parameters used for hadronic cascade shower is generated newline ! For you may give as as or em quick generation of AS for heavy primaries is tried See chookASbyH f character* Generate2 don t touch this for skeleton flesh use integer MagBrem no magnetic bremsstrahlung is considered newline ! if and Ee energy loss due to magnetic brems is considered newline ! if and Ee MagBremEmin |
◆ MagPairEmin
| ! Parameters used for hadronic cascade shower is generated newline ! For you may give as as or em quick generation of AS for heavy primaries is tried See chookASbyH f character* Generate2 don t touch this for skeleton flesh use integer MagBrem no magnetic bremsstrahlung is considered newline ! if and Ee energy loss due to magnetic brems is considered newline ! if and Ee real sampling of gamma is performed WaitRatio ! must be made small so that WaitRatio* E0 sim MagBremEmin integer MagPair no magnetic pair creation is considered newline ! if and Eg MagPairEmin |
◆ this
| ! Parameters used for hadronic cascade shower is generated newline ! For you may give as as or em quick generation of AS for heavy primaries is tried See chookASbyH f character* Generate2 don t touch this for skeleton flesh use integer MagBrem no magnetic bremsstrahlung is considered newline ! if and Ee energy loss due to magnetic brems is considered newline ! if and Ee real sampling of gamma is performed WaitRatio ! must be made small so that WaitRatio* E0 sim MagBremEmin integer MagPair no magnetic pair creation is considered newline ! if and Eg real sampling is the LPM effect is considered when Ee LpmBremEmin for electrons and ! Eg LpmPairEmin for gamma rays real* MagBremEmin E this |
