iceCube.uhe.neutrinoModel
public class NeutrinoFlux extends java.lang.Object implements Function
UHE Neutrino fluxes based on the following moels are calculated from the table.
The Astrophysical Journal 479 547-559 (1997) |
Phys.Rev.Lett. 81 5505 (1998) |
Phys.Rev.Rev. D 59 043504 (1998) |
Phys.Rev.Rev. D 66 063004 (2002) |
Astropart. Phys. 34 106-115 (2010) |
JCAP 10 013 (2010) |
Phys Rev D 90 023007 (2014) |
Phys Rev D 90 103005 (2014) |
Note that NO NEUTRINO OSCILATION was considered in these models. One can access the original flux with getEFlux and/or getDFDLogE method. The flux at the earth surface after propagation in space with neutrino oscillation effect are also calculated based on the recent result of the oscillation parameters. One can access the flux after having the oscillation effect with getEFluxwzOsci and/or getDFDLogEwzOsci. The tables to contain the flux data is stored in $JAVADIR/classes/icecube/uhe/neutrinoModel which are read out by this class. Usage: NeutrinoFlux model-parameter model-parameter 1 the GZK neutrinos m=0 Zmax = 2 2 the GZK neutrinos m=2 Zmax = 2 3 the GZK neutrinos m=2 Zmax = 4 4 the GZK neutrinos m=4 Zmax = 4 5 the GZK neutrinos m=4 Zmax = 5 gamma=1.5 6 the GZK neutrinos m=7 Zmax = 5 gamma=1.5 7 the Z-burst 8 the Top Down (SUSY) 9 the Top Down (QCD) 10 the GZK neutrinos (by Sigl) m=3 Zmax=2 gamma=1 Emax=100ZeV 11 the GZK neutrinos (by Sigl) m=5 Zmax=3 gamma=2 Emax=10ZeV 12 the GZK neutrinos (by Ahles, Francis et al) Emin 10EeV best fit with the Fermi constraint m=4.6 Zmax=2 gamma=2.5 Emax = 1ZeV 13 the GZK neutrinos (by Ahles, Francis et al) Emax 10EeV max fit with the Fermi constraint m=4.4 Zmax=2 gamma=2.1 Emax = 1ZeV 14 the GZK neutrinos (by Ahles, Francis et al) Emax 10EeV min fit with the Fermi constraint m=2.0 Zmax=2 gamma=2.88 Emax = 1ZeV 15 the GZK neutrinos (by Kotera) Uniform, Emax 316 EeV 16 the GZK neutrinos (by Kotera) SFR1, Emax 316 EeV 17 the GZK neutrinos (by Kotera) GRB1, Emax 316 EeV 18 the GZK neutrinos (by Kotera) FR2, Emax 316 EeV 19 the GZK neutrinos (by Ahles, Francis et al) Emin 3EeV max fit with the Fermi constraint m=5.35 Zmax=2 gamma=2.28 Emax = 1ZeV 20 the GZK neutrinos (by Ahles, Francis et al) Emin 3EeV min fit with the Fermi constraint m=2.0 Zmax=2 gamma=2.63 Emax = 1ZeV 21 the GZK neutrinos (by Ahles, Francis et al) Emin 3EeV best fit with the Fermi constraint m=4.05 Zmax=2 gamma=2.47 Emax = 1ZeV 22 the GZK neutrinos (by Kotera) no evolution, CMB only, Emax 316 EeV 23 the GZK neutrinos (by Ahles, Francis et al) maximal with the Fermi constraint m=7 Zmax=4 gamma=2.0 Emax=3ZeV 24 The baseline E-2 flux - J(E)E^2 = 10^-8 [GeV/cm^2 sec sr] per neutrino flavor. 25 GZK by simProp (Alosio et al) SFR, KneiskeEBL 26 GZK by simProp (Alosio et al) SFR, SteckerEBL 26 GZK by simProp (Alosio et al) SFR, CMB only 28 GZK by simProp (Alosio et al) FR2, KneiskeEBL 29 GZK by simProp (Alosio et al) FR2, SteckerEBL 30 GZK by simProp (Alosio et al) FR2, CMB only 31 AGN neutrinos (Murase et al) gamma = 2.0 CR loading factor 10 32 AGN neutrinos (Murase et al) gamma = 2.3 CR loading factor 10 33 Newborn pulsar neutrinos (Ke, Kumiko, Angela) SFR 34 Newborn pulsar neutrinos (Ke, Kumiko, Angela) uniform 35 AGN Blazars (Padovani et al) HBL only Y_nu_gamma=0.8 36 AGN Blazars (Padovani et al) all Y_nu_gamma=0.8 37 the GZK neutrinos (by Ahles, Francis et al) Emin 1EeV best fit with the Fermi constraint m=3.2 Zmax=2 gamma=2.52 Emax = 1ZeV particleID 1 nu-e 2 nu-mu 3 nu-tau (No nu-tau in the GZK model)
Constructor and 説明 |
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NeutrinoFlux(int model)
Constructor: Reads out from the table stored in iceCube/uhe/neutrinoModel
logE [eV] dF/dE E^2 [eV/cm^2 sec sr].
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Modifier and Type | Method and 説明 |
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double |
getDFDLogE(double logEnergy,
int particleID)
calculate the log differential Flux dF/dLogE [/cm^2 sec sr]
logEnergy [GeV]
particleID
1 nu-e
2 nu-mu
3 nu-tau (No nu-tau in the GZK model)
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double[] |
getDFDLogEwzOsci(double logEnergy)
Calculate the log differential Flux dF/dLogE [/cm^2 sec sr]
after the propagation in the universe (with taking into account
the neutrino oscillation)
input: logEnergy [GeV]
output: neutrino fluxes after neutrino oscillation
(0: nu_e, 1:nu_mu, 2:nu_tau)
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double |
getDFDLogEwzOsci(double logEnergy,
int particleID)
Calculate the log differential Flux dF/dLogE [/cm^2 sec sr]
after the propagation in the universe (with taking into account
the neutrino oscillation)
Calculation is based on a paper of J.
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double |
getEflux()
Get the normalization E^2dF/dE [GeV/cm2 sec sr] for the power law model (model ID 24)
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double |
getEFlux(double logEnergy,
int particleID)
calculate the differential Energy Flux [GeV /cm^2 sec sr]
logEnergy [GeV]
particleID
1 nu-e
2 nu-mu
3 nu-tau (No nu-tau in the GZK model)
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double[] |
getEFluxwzOsci(double logEnergy)
Calculate the differential Energy Flux [GeV /cm^2 sec sr]
after the propagation in the universe (with taking into account
the neutrino oscillation)
input: logEnergy [GeV]
output: neutrino fluxes after neutrino oscillation
(0: nu_e, 1:nu_mu, 2:nu_tau)
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double |
getEFluxwzOsci(double logEnergy,
int particleID)
Calculate the differential Energy Flux [GeV /cm^2 sec sr]
after the propagation in the universe (with taking into account
the neutrino oscillation)
input: logEnergy [GeV]
particleID
1 nu-e
2 nu-mu
3 nu-tau (No nu-tau in the GZK model)
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double |
getEnergyBase()
Set the base energy [GeV] to define normalization E^2dF/dE [GeV/cm2 sec sr]
for the power law model (model ID 24)
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protected double[] |
getFluxwzOsci(double logEnergy,
double nueflux,
double numuflux,
double nutauflux)
Calculate the neutrino flux at the earth surface after propgation in space
with neutrino oscillation.
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double |
getFunction(int functionIndex,
double[] parameters,
double x)
Interface to Integration class.
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double |
getLogEmax()
Return the logEmax[GeV] setted for the power law model (model ID 24)
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double |
getPowerLawIndex()
Get the powerlaw index for the power law model (model ID 24)
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boolean |
isPowerLaw()
tell if the setted model is a powerlaw model or not
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void |
setEflux(double eFlux)
Set the normalization E^2dF/dE [GeV/cm2 sec sr] for the power law model (model ID 24)
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void |
setEnergyBase(double eBase)
Set the base energy [GeV] to define normalization E^2dF/dE [GeV/cm2 sec sr]
for the power law model (model ID 24)
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void |
setLogEmax(double logEnergy)
Set the logEmax[GeV] for the power law model (model ID 24)
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void |
setPowerLawIndex(double gamma)
Set the powerlaw index for the power law model (model ID 24)
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public NeutrinoFlux(int model) throws java.io.IOException
java.io.IOException
public void setLogEmax(double logEnergy)
public double getLogEmax()
public void setEflux(double eFlux)
public double getEflux()
public void setPowerLawIndex(double gamma)
public double getPowerLawIndex()
public boolean isPowerLaw()
public void setEnergyBase(double eBase)
public double getEnergyBase()
public double getEFlux(double logEnergy, int particleID)
calculate the differential Energy Flux [GeV /cm^2 sec sr] logEnergy [GeV] particleID 1 nu-e 2 nu-mu 3 nu-tau (No nu-tau in the GZK model)
public double getDFDLogE(double logEnergy, int particleID)
calculate the log differential Flux dF/dLogE [/cm^2 sec sr] logEnergy [GeV] particleID 1 nu-e 2 nu-mu 3 nu-tau (No nu-tau in the GZK model)
protected double[] getFluxwzOsci(double logEnergy, double nueflux, double numuflux, double nutauflux)
Calculate the neutrino flux at the earth surface after propgation in space with neutrino oscillation. Calculation is based on a paper of J. Jones et al., PRD, 69, 033004 (2004) Note that the mixing between nu_e and nu_tau is known to be very small, so the mixing is ignored. input: logEnergy [GeV], nu_e flux before neutrino oscillation, nu_mu flux before neutrino oscillation, nu_tau flux before neutrino oscillation output: neutrino fluxes after neutrino oscillation (0: nu_e, 1:nu_mu, 2:nu_tau)
public double[] getEFluxwzOsci(double logEnergy)
Calculate the differential Energy Flux [GeV /cm^2 sec sr] after the propagation in the universe (with taking into account the neutrino oscillation) input: logEnergy [GeV] output: neutrino fluxes after neutrino oscillation (0: nu_e, 1:nu_mu, 2:nu_tau)
public double getEFluxwzOsci(double logEnergy, int particleID)
Calculate the differential Energy Flux [GeV /cm^2 sec sr] after the propagation in the universe (with taking into account the neutrino oscillation) input: logEnergy [GeV] particleID 1 nu-e 2 nu-mu 3 nu-tau (No nu-tau in the GZK model)
public double[] getDFDLogEwzOsci(double logEnergy)
Calculate the log differential Flux dF/dLogE [/cm^2 sec sr] after the propagation in the universe (with taking into account the neutrino oscillation) input: logEnergy [GeV] output: neutrino fluxes after neutrino oscillation (0: nu_e, 1:nu_mu, 2:nu_tau)
public double getDFDLogEwzOsci(double logEnergy, int particleID)
Calculate the log differential Flux dF/dLogE [/cm^2 sec sr] after the propagation in the universe (with taking into account the neutrino oscillation) Calculation is based on a paper of J. Jones et al., PRD, 69, 033004 (2004) Note that the mixing between nu_e and nu_tau is known to be very small, so the mixing is ignored. input: logEnergy [GeV] particleID 1 nu-e 2 nu-mu 3 nu-tau (No nu-tau in the GZK model)
public double getFunction(int functionIndex, double[] parameters, double x)
getFunction
インタフェース {1} 内の {0} Function