| 1 |
pamela |
1.1 |
C*****This subroutine fills the common NeutronsGR: Number_N, Neut_En(3), |
| 2 |
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C teta_n(3), fi_n(3), |
| 3 |
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C*****where |
| 4 |
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C*****Number_N - number of neutrons in case of Gigantic resonance |
| 5 |
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C (Number_N=0, if no); |
| 6 |
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C*****NeutE_n(i) - energy of each generated neutron, MeV |
| 7 |
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C*****teta_n(i) - teta (polar) angle in reference coordinate system |
| 8 |
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C*****fi_n(i) - fi (azimuth) angle in reference coordinate system Input |
| 9 |
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C parameters from GEANT: Step - GEANT step, cm En-gamma - gamma |
| 10 |
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C energy in tungsten, GeV px_gamma, py_gamma, pz_gamma - gamma |
| 11 |
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C momentum projections, GeV |
| 12 |
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subroutine GPGRES(Step, En_g, px_g, py_g, pz_g) |
| 13 |
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| 14 |
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integer i |
| 15 |
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real En_exc |
| 16 |
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real cos_teta, sin_teta, cos_fi, sin_fi, En_n, alfa_n, beta_n |
| 17 |
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| 18 |
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C Input parameters |
| 19 |
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* Energy of gamma, in GeV |
| 20 |
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real En_gamma |
| 21 |
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* Gamma momentum projections, multiplied by c, in GeV |
| 22 |
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real px_gamma, py_gamma, pz_gamma |
| 23 |
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* GEANT step, in cm |
| 24 |
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real Step |
| 25 |
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| 26 |
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common/bind/En_bind(3) |
| 27 |
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#include "gpgneut.inc" |
| 28 |
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c |
| 29 |
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* |
| 30 |
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* Let's trasnform energy and momentum in MeV. Remember, GEANT is GeV |
| 31 |
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* |
| 32 |
cafagna |
1.2 |
* open(77,file='testgig.dat',access='append') |
| 33 |
pamela |
1.1 |
En_gamma=En_g/1000. |
| 34 |
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px_gamma=px_g/1000. |
| 35 |
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py_gamma=py_g/1000. |
| 36 |
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pz_gamma=pz_g/1000. |
| 37 |
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* |
| 38 |
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* Exciting energy of nucleus in Gigantic resonance, MeV |
| 39 |
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En_exc=En_gamma |
| 40 |
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Number_N=0 |
| 41 |
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do i=1,3 |
| 42 |
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Neut_En(i)=0. |
| 43 |
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teta_n(i)=0. |
| 44 |
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fi_n(i)=0. |
| 45 |
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enddo |
| 46 |
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| 47 |
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C Simulate number of neutrons in Gygantic resonance process |
| 48 |
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C (Number_n=0 if no interaction) |
| 49 |
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call GRESsimulate(En_gamma, Step, Number_N) |
| 50 |
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| 51 |
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if (Number_N.gt.0) then |
| 52 |
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cos_teta=pz_gamma/sqrt(px_gamma**2+py_gamma**2+pz_gamma**2) |
| 53 |
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sin_teta=sqrt(1.-cos_teta**2) |
| 54 |
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cos_fi=px_gamma/sqrt(px_gamma**2+py_gamma**2) |
| 55 |
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sin_fi=py_gamma/sqrt(px_gamma**2+py_gamma**2) |
| 56 |
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| 57 |
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do i=1, Number_N |
| 58 |
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if (En_exc.gt.En_bind(i)) then |
| 59 |
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call SpectrumSpace(Number_N, i, En_exc, |
| 60 |
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& cos_teta, sin_teta, cos_fi, sin_fi, |
| 61 |
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& En_n, alfa_n, beta_n) |
| 62 |
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Neut_En(i)=En_n |
| 63 |
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teta_n(i)=alfa_n |
| 64 |
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fi_n(i)=beta_n |
| 65 |
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En_exc=En_exc-En_bind(i)-En_n |
| 66 |
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endif |
| 67 |
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enddo |
| 68 |
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| 69 |
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endif |
| 70 |
cafagna |
1.2 |
* write(77,*) Number_N, step, en_gamma |
| 71 |
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* close(77) |
| 72 |
pamela |
1.1 |
RETURN |
| 73 |
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end |
| 74 |
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| 75 |
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c************************************************************************ |
| 76 |
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************************************************************************* |
| 77 |
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C*****Simulate generated number of |
| 78 |
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C*****neutrons |
| 79 |
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C****************************** |
| 80 |
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subroutine GRESsimulate(En_gamma, Step, Number_N) |
| 81 |
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c Output parameter: Number_N (as default Number_N=0) |
| 82 |
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real En_gamma, Step |
| 83 |
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integer Number_N |
| 84 |
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| 85 |
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real Sigma |
| 86 |
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real*4 tmp |
| 87 |
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real Lambda1, Lambda2, Lambda3 |
| 88 |
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| 89 |
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#include "gpgsigma.inc" |
| 90 |
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| 91 |
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if ((En_gamma.gt.9.097).and.(En_gamma.lt.28.608)) then |
| 92 |
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CCCCC Calculate Lambda1 |
| 93 |
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Sigma=-1. |
| 94 |
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do i=1,63 |
| 95 |
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if ((En_gamma.ge.energy1(i)).and.(En_gamma.lt.energy1(i+1))) |
| 96 |
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& Sigma=cross1(i)+(cross1(i+1)-cross1(i))* |
| 97 |
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& (En_gamma-energy1(i))/ |
| 98 |
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& (energy1(i+1)-energy1(i)) |
| 99 |
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enddo |
| 100 |
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if (Sigma.le.0.) then |
| 101 |
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Lambda1=1000. |
| 102 |
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else |
| 103 |
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1 call GRNDM(tmp,1) |
| 104 |
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if ((tmp.lt.1.E-8).or.(tmp.gt.(1.-1.E-8))) goto 1 |
| 105 |
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Lambda1=-log(1.-tmp)/(Sigma*1.E-27*6.31*1.E22) |
| 106 |
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endif |
| 107 |
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CCCCCCCalculate Lambda2 |
| 108 |
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Sigma=-1. |
| 109 |
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do i=1,61 |
| 110 |
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if ((En_gamma.ge.energy2(i)).and.(En_gamma.lt.energy2(i+1))) |
| 111 |
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& Sigma=cross2(i)+(cross2(i+1)-cross2(i))* |
| 112 |
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& (En_gamma-energy2(i))/ |
| 113 |
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& (energy2(i+1)-energy2(i)) |
| 114 |
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enddo |
| 115 |
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if (Sigma.le.0.) then |
| 116 |
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Lambda2=1000. |
| 117 |
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else |
| 118 |
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2 call GRNDM(tmp,1) |
| 119 |
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if ((tmp.lt.1.E-8).or.(tmp.gt.(1.-1.E-8))) goto 2 |
| 120 |
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Lambda2=-log(1.-tmp)/(Sigma*1.E-27*6.31*1.E22) |
| 121 |
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endif |
| 122 |
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| 123 |
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CCCCCCCalculate Lambda3 |
| 124 |
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Sigma=-1. |
| 125 |
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do i=1,26 |
| 126 |
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if ((En_gamma.ge.energy3(i)).and.(En_gamma.lt.energy3(i+1))) |
| 127 |
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& Sigma=cross3(i)+(cross3(i+1)-cross3(i))* |
| 128 |
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& (En_gamma-energy3(i))/ |
| 129 |
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& (energy3(i+1)-energy3(i)) |
| 130 |
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enddo |
| 131 |
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if (Sigma.le.0.) then |
| 132 |
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Lambda3=1000. |
| 133 |
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else |
| 134 |
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3 call GRNDM(tmp,1) |
| 135 |
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if ((tmp.lt.1.E-8).or.(tmp.gt.(1.-1.E-8))) goto 3 |
| 136 |
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Lambda3=-log(1.-tmp)/(Sigma*1.E-27*6.31*1.E22) |
| 137 |
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endif |
| 138 |
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| 139 |
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if (Lambda1.eq.MIN(Lambda1, Lambda2, Lambda3, Step)) Number_N=1 |
| 140 |
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if (Lambda2.eq.MIN(Lambda1, Lambda2, Lambda3, Step)) Number_N=2 |
| 141 |
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if (Lambda3.eq.MIN(Lambda1, Lambda2, Lambda3, Step)) Number_N=3 |
| 142 |
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endif |
| 143 |
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RETURN |
| 144 |
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end |
| 145 |
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| 146 |
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c************************************************************************ |
| 147 |
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c************************************************************************ |
| 148 |
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******Simulate neutron energy and flight direction*********************** |
| 149 |
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| 150 |
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subroutine SpectrumSpace(Number_N, Num, En_exc, |
| 151 |
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& cos_teta, sin_teta, cos_fi, sin_fi, En_n, alfa_n, beta_n) |
| 152 |
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c Output parameters: En_n, alfa_n, beta_n |
| 153 |
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common/bind/En_bind(3) |
| 154 |
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| 155 |
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real tmp(2) |
| 156 |
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real Pi, Temperature, lev_dens, cos_alfa, sin_alfa, beta |
| 157 |
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real cos_alfa_n, cos_beta_n, sin_beta_n |
| 158 |
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integer Number_N, Num |
| 159 |
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| 160 |
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real En_exc |
| 161 |
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real cos_teta, sin_teta, cos_fi, sin_fi, En_n, alfa_n, beta_n |
| 162 |
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| 163 |
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Pi=4.*atan(1.) |
| 164 |
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if (Number_N.eq.1) then |
| 165 |
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En_n=En_exc-En_bind(1) |
| 166 |
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| 167 |
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else if ((Number_N.eq.2).and.(Num.eq.1)) then |
| 168 |
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C************************************************************************ |
| 169 |
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C SIMULATION OF NEUTRON EVAPORATION SPECTRUM The reference book |
| 170 |
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C is: V.C. Barashenkov, V.D. Toneev, "The interactions of high |
| 171 |
|
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C energy particles and atomic nuclei with nuclei", in Russian |
| 172 |
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C Calculation of density levels parameter (see (6.31) from reference |
| 173 |
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C book) |
| 174 |
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lev_dens=0.085*184. |
| 175 |
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C Calculation of nucleus temperature (see (6.30) from reference book) |
| 176 |
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C (see (6.64) and comments after) |
| 177 |
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Temperature=sqrt((En_exc-En_bind(Num))/lev_dens) |
| 178 |
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| 179 |
|
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C Neutron evaporation energy spectrum simulation by exception method |
| 180 |
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4 call GRNDM(tmp,2) |
| 181 |
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C The average binding energy of neutron |
| 182 |
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x_tmp=(En_exc-En_bind(1)-En_bind(2))*tmp(1) |
| 183 |
|
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y_tmp=(exp(-1.)/Temperature)*tmp(2) |
| 184 |
|
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if (y_tmp.gt.((x_tmp/Temperature**2)*exp(-x_tmp/Temperature))) |
| 185 |
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& goto 4 |
| 186 |
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En_n=x_tmp |
| 187 |
|
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else if ((Number_N.eq.2).and.(Num.eq.2)) then |
| 188 |
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En_n=En_exc-En_bind(2) |
| 189 |
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else if ((Number_N.eq.3).and.(Num.eq.1)) then |
| 190 |
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C************************************************************************ |
| 191 |
|
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C SIMULATION OF NEUTRON EVAPORATION SPECTRUM The reference book is: |
| 192 |
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C V.C. Barashenkov, V.D. Toneev, "The interactions of high energy |
| 193 |
|
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C particles and atomic nuclei with nuclei", in Russian Calculation |
| 194 |
|
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C of density levels parameter (see (6.31) from reference book) |
| 195 |
|
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lev_dens=0.085*184. |
| 196 |
|
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C Calculation of nucleus temperature (see (6.30) from reference book) |
| 197 |
|
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C (see (6.64) and comments after) |
| 198 |
|
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Temperature=sqrt((En_exc-En_bind(Num))/lev_dens) |
| 199 |
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|
| 200 |
|
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C Neutron evaporation energy spectrum simulation by exception method |
| 201 |
|
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5 call GRNDM(tmp,2) |
| 202 |
|
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C Average binding energy of neutron |
| 203 |
|
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x_tmp=(En_exc-En_bind(1)-En_bind(2)-En_bind(3))*tmp(1) |
| 204 |
|
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y_tmp=(exp(-1.)/Temperature)*tmp(2) |
| 205 |
|
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if (y_tmp.gt.((x_tmp/Temperature**2)*exp(-x_tmp/Temperature))) |
| 206 |
|
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& goto 5 |
| 207 |
|
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En_n=x_tmp |
| 208 |
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|
| 209 |
|
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else if ((Number_N.eq.3).and.(Num.eq.2)) then |
| 210 |
|
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C************************************************************************ |
| 211 |
|
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C SIMULATION OF NEUTRON EVAPORATION SPECTRUM The reference book |
| 212 |
|
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C is: V.C. Barashenkov, V.D. Toneev, "The interactions of high |
| 213 |
|
|
C energy particles and atomic nuclei with nuclei", in Russian |
| 214 |
|
|
C Calculation of density levels parameter (see (6.31) from reference |
| 215 |
|
|
C book) |
| 216 |
|
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lev_dens=0.085*183. |
| 217 |
|
|
C Calculation of nucleus temperature (see (6.30) from reference book) |
| 218 |
|
|
C (see (6.64) and comments after) |
| 219 |
|
|
Temperature=sqrt((En_exc-En_bind(Num))/lev_dens) |
| 220 |
|
|
|
| 221 |
|
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C Neutron evaporation energy spectrum simulation by exception method |
| 222 |
|
|
6 call GRNDM(tmp,2) |
| 223 |
|
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C Average binding energy of neutron |
| 224 |
|
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x_tmp=(En_exc-En_bind(2)-En_bind(3))*tmp(1) |
| 225 |
|
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y_tmp=(exp(-1.)/Temperature)*tmp(2) |
| 226 |
|
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if (y_tmp.gt.((x_tmp/Temperature**2)*exp(-x_tmp/Temperature))) |
| 227 |
|
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& goto 6 |
| 228 |
|
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En_n=x_tmp |
| 229 |
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|
| 230 |
|
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else if ((Number_N.eq.3).and.(Num.eq.3)) then |
| 231 |
|
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En_n=En_exc-En_bind(3) |
| 232 |
|
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| 233 |
|
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endif |
| 234 |
|
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C************************************************************************ |
| 235 |
|
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C Neutron direction simulation in gamma coordinate system |
| 236 |
|
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call GRNDM(tmp,2) |
| 237 |
|
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cos_alfa=-1.+2.*tmp(1) |
| 238 |
|
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beta=2.*Pi*tmp(2) |
| 239 |
|
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sin_alfa=sqrt(1.-cos_alfa**2) |
| 240 |
|
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C Return to the GEANT reference coordinate system |
| 241 |
|
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cos_alfa_n=-sin_alfa*cos(beta)*(sin_teta)+cos_alfa*(cos_teta) |
| 242 |
|
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cos_beta_n=sin_alfa*cos(beta)*(cos_teta*cos_fi)- |
| 243 |
|
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& sin_alfa*sin(beta)*(sin_fi)+cos_alfa*(sin_teta*cos_fi) |
| 244 |
|
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sin_beta_n=sin_alfa*cos(beta)*(cos_teta*sin_fi)+ |
| 245 |
|
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& sin_alfa*sin(beta)*(cos_fi)+cos_alfa*(sin_teta*sin_fi) |
| 246 |
|
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if (abs(cos_beta_n).lt.1.E-6) cos_beta_n=0. |
| 247 |
|
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if (abs(sin_beta_n).lt.1.E-6) sin_beta_n=0. |
| 248 |
|
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if ((cos_beta_n.eq.0.).and.(sin_beta_n.eq.0.)) beta_n=0. |
| 249 |
|
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| 250 |
|
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alfa_n=acos(cos_alfa_n) |
| 251 |
|
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if ((cos_beta_n.ge.0.).and.(sin_beta_n.gt.0.)) |
| 252 |
|
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& beta_n=atan(sin_beta_n/cos_beta_n) |
| 253 |
|
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if ((cos_beta_n.ge.0.).and.(sin_beta_n.lt.0.)) |
| 254 |
|
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& beta_n=2.*Pi+atan(sin_beta_n/cos_beta_n) |
| 255 |
|
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if ((cos_beta_n.lt.0.).and.(sin_beta_n.le.0.)) |
| 256 |
|
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& beta_n=Pi+atan(sin_beta_n/cos_beta_n) |
| 257 |
|
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if ((cos_beta_n.lt.0.).and.(sin_beta_n.ge.0.)) |
| 258 |
|
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& beta_n=Pi+atan(sin_beta_n/cos_beta_n) |
| 259 |
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| 260 |
|
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RETURN |
| 261 |
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END |
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