def dRdE_nu(E_r,t,sol,E_nu,Flux,Nuc):
N = Nuc.NumberOfNeutrons
Z = Nuc.NumberOfProtons
Q_W = 1.0*N-(1-4.0*sinTheta_Wsq)*Z # weak nuclear hypercharge
m_N_GeV = 0.93141941*(N+Z) # nucleus mass in GeV
m_N_keV = m_N_GeV*1.0e6 # nucleus mass in keV
dRdE = zeros(shape=shape(E_r))
FF = LabFuncs.FormFactorHelm(E_r,N+Z)**2.0
ne = size(E_r)
if Flux[1]>0.0:
for i in range(0,ne):
diff_sigma = (G_F_GeV**2.0 /(4.0*pi))*(Q_W**2.0)*m_N_GeV*(1.0 \
-(m_N_keV*E_r[i])/(2.0*(E_nu*1000.0)**2.0))*\
(0.197e-13)**2.0*(1.0e-6)*1000.0/(1.0*N+1.0*Z)*(N_A)
diff_sigma[diff_sigma<0.0] = 0.0
dRdE[i] = trapz(diff_sigma*Flux*FF[i],x=E_nu)
else:
for i in range(0,ne):
diff_sigma = (G_F_GeV**2.0 /(4.0*pi))*(Q_W**2.0)*m_N_GeV*(1.0 \
-(m_N_keV*E_r[i])/(2.0*(E_nu[0]*1000.0)**2.0))*\
(0.197e-13)**2.0*(1.0e-6)*1000.0/(1.0*N+1.0*Z)*(N_A)
if diff_sigma>0:
dRdE[i] = diff_sigma*Flux[0]*E_nu[0] # for monochromatic nu's
if sol:
fMod = LabFuncs.EarthSunDistanceMod(t)
else:
fMod = 1.0
# Convert into /ton/year/keV
dRdE = fMod*dRdE*(365.0*3600.0*24.0*1000.0)
return dRdE
def dRdEe_nu(E_r, t, sol, E_nu, Flux, Atom, flav):
N = Atom.NumberOfNeutrons
Z = Atom.NumberOfProtons
Q_W = 1.0 * N - (1 - 4.0 * sinTheta_Wsq) * Z # weak nuclear hypercharge
m_N_GeV = 0.93141941 * (N + Z) # nucleus mass in GeV
m_N_keV = m_N_GeV * 1.0e6 # nucleus mass in keV
m_e_GeV = 5.109989461e-4
ne = size(E_r)
if sol:
fMod = LabFuncs.EarthSunDistanceMod(t)
else:
fMod = 1.0
gV = array([
2 * sinTheta_Wsq + 0.5, 2 * sinTheta_Wsq - 0.5, 2 * sinTheta_Wsq - 0.5,
2 * sinTheta_Wsq + 0.5, 2 * sinTheta_Wsq - 0.5, 2 * sinTheta_Wsq - 0.5
])
gA = array([0.5, -0.5, -0.5, -0.5, 0.5, 0.5])
T = E_r / 1000 # MeV
Tmax = 2 * E_nu**2.0 / (2 * E_nu + m_e_GeV * 1000)
dR = 0.0
for ii in arange(0, 6)[flav > 0]:
dRdE = zeros(shape=ne)
As = (gV[ii] + gA[ii])**2.0
Bs = (gV[ii] - gA[ii])**2.0
Cs = (gA[ii]**2.0 - gV[ii]**2.0)
if Flux[1] > 0.0:
for i in range(0, ne):
diff_sigma = (G_F_GeV**2.0 * m_e_GeV /
(2 * pi)) * (As + Bs *
(1 - T[i] / E_nu)**2.0 + Cs * 1000 *
m_e_GeV * T[i] / E_nu**2.0)
diff_sigma *= (0.197e-13)**2.0 * (1.0e-6) * 1000.0 / (
1.0 * N + 1.0 * Z) * (N_A)
diff_sigma[T[i] > Tmax] = 0.0
dRdE[i] = trapz(diff_sigma * Flux, x=E_nu)
else:
diff_sigma = (G_F_GeV**2.0 * m_e_GeV /
(2 * pi)) * (As + Bs * (1 - T / E_nu[0])**2.0 +
Cs * 1000 * m_e_GeV * T / E_nu[0]**2.0)
diff_sigma *= (0.197e-13)**2.0 * (1.0e-6) * 1000.0 / (
1.0 * N + 1.0 * Z) * (N_A)
diff_sigma[T > Tmax[0]] = 0.0
dRdE = diff_sigma * Flux[0] * E_nu[0] * (
diff_sigma > 0.0) # for monochromatic nu's
# Convert into /ton/year/keV
dRdE = fMod * dRdE * (365.0 * 3600.0 * 24.0 * 1000.0)
dRdE = dRdE * Z * flav[ii]
dR += dRdE
return dR
def dRdEdO_solarnu(E,t,E_nu,Flux,Nuc,Loc): # Directional CEnuNS for Solar
N = Nuc.NumberOfNeutrons
Z = Nuc.NumberOfProtons
Q_W = N-(1-4.0*sinTheta_Wsq)*Z # weak nuclear hypercharge
m_N_GeV = 0.93141941*(N+Z) # nucleus mass in GeV
m_N_keV = m_N_GeV*1.0e6 # nucleus mass in keV
E_nu_keV = E_nu*1e3
E_r = sqrt(E[:,0]**2 + E[:,1]**2 + E[:,2]**2) # Recoil energy
x = zeros(shape=shape(E))
x_sun = zeros(shape=shape(E))
x[:,0] = E[:,0]/E_r # Recoil direction
x[:,1] = E[:,1]/E_r
x[:,2] = E[:,2]/E_r
ne =size(E_r)
dRdEdO = zeros(shape=ne)
for i in range(0,ne):
x_sun[i,:] = LabFuncs.SolarDirection(t[i],Loc)
cos_th_sun = -(x_sun[:,0]*x[:,0]+x_sun[:,1]*x[:,1]+x_sun[:,2]*x[:,2])
FF = LabFuncs.FormFactorHelm(E_r,N+Z)**2.0
# CHROMATIC NEUTRINOS
if Flux[1]>0.0:
E_max = 2*m_N_keV*E_nu_keV[-1]**2.0/(m_N_keV+E_nu_keV[-1])**2
i_range = range(0,ne)*(E_r<=E_max)
i_sel = i_range[i_range!=0]
for i in i_sel:
costh = cos_th_sun[i]
E_nu_min = sqrt(m_N_keV*E_r[i]/2.0)
if costh>(E_nu_min/m_N_keV):
Eps = 1.0/(costh/E_nu_min - 1.0/m_N_keV)
diff_sigma = (G_F_GeV**2/(4*pi))*Q_W**2*m_N_GeV*\
(1-(m_N_keV*E_r[i])/(2*Eps**2))*(0.197e-13)**2.0\
*1e-6*1000/(N+1.0*Z)*(N_A)
Eps = Eps*(Eps>E_nu_min)
Eps = Eps*(Eps<E_nu_keV[-1])
F_value = interp(Eps,E_nu_keV,Flux)
dRdEdO[i] = diff_sigma*F_value*Eps**2.0/(1000*E_nu_min)*FF[i] # /kg/keV
# MONOCHROMATIC NEUTRINOS
else:
E_max = 2*m_N_keV*E_nu_keV[0]**2.0/(m_N_keV+E_nu_keV[0])**2
i_range = range(0,ne)*(E_r<=E_max)
i_sel = i_range[i_range!=0]
for i in i_sel:
costh = cos_th_sun[i]
E_nu_min = sqrt(m_N_keV*E_r[i]/2.0)
costh_r = ((E_nu_keV[0]+m_N_keV)/E_nu_keV[0])*sqrt(E_r[i]/(2*m_N_keV))
# just need to accept angles close enough to costh_r to be accurate
# around 0.01 is enough to be disguised by most angular resolutions
if abs((costh)-(costh_r))<0.01:
Eps = E_nu_keV[0]
diff_sigma = (G_F_GeV**2/(4*pi))*Q_W**2*m_N_GeV*\
(1-(m_N_keV*E_r[i])/(2*Eps**2))*(0.197e-13)**2.0\
*1e-6*1000/(N+1.0*Z)*(N_A)*FF[i]
dRdEdO[i] = diff_sigma*(Flux[0]/1000.0)*E_nu_keV[0] # /kg/keV
fMod = LabFuncs.EarthSunDistanceMod(t)
dRdEdO = fMod*dRdEdO*3600*24*365*1000/(2*pi) # /ton/year
return dRdEdO