NuRadioMC.SignalGen.askaryan module

NuRadioMC.SignalGen.askaryan.set_log_level(level)[source]

NuRadioMC.SignalGen.askaryan.get_time_trace(energy, theta, N, dt, shower_type, n_index, R, model, interp_factor=None, interp_factor2=None, same_shower=False, seed=None, full_output=False, **kwargs)[source]

returns the Askaryan pulse in the time domain of the eTheta component

We implement only the time-domain solution and obtain the frequency spectrum via FFT (with the standard normalization of NuRadioMC). This approach assures that the units are interpreted correctly. In the time domain, the amplitudes are well defined and no details about fourier transform normalizations needs to be known by the user.

Parameters:

energyfloat

energy of the shower

theta: float

viewangle: angle between shower axis (neutrino direction) and the line of sight between interaction and detector

Nint

number of samples in the time domain

dt: float

time bin width, i.e. the inverse of the sampling rate

shower_type: string (default “HAD”)

type of shower, either “HAD” (hadronic), “EM” (electromagnetic) or “TAU” (tau lepton induced) note that TAU showers are currently only implemented in the ARZ2019 model

n_index: float

index of refraction at interaction vertex

R: float

distance from vertex to observer

model: string

specifies the signal model

ZHS1992: the original ZHS parametrization from E. Zas, F. Halzen, and T. Stanev, Phys. Rev. D 45, 362 (1992), https://doi.org/10.1103/PhysRevD.45.362, this parametrization does not contain any phase information
Alvarez2000: parameterization based on ZHS mainly based on J. Alvarez-Muniz, R. A. Vazquez, and E. Zas, Calculation methods for radio pulses from high energy showers, Physical Review D62 (2000) https://doi.org/10.1103/PhysRevD.84.103003
Alvarez2009: parameterization based on ZHS from J. Alvarez-Muniz, W. R. Carvalho, M. Tueros, and E. Zas, Coherent cherenkov radio pulses from hadronic showers up to EeV energies, Astroparticle Physics 35 (2012), no. 6 287 – 299 and J. Alvarez-Muniz, C. James, R. Protheroe, and E. Zas, Thinned simulations of extremely energetic showers in dense media for radio applications, Astroparticle Physics 32 (2009), no. 2 100 – 111
HCRB2017: analytic model from J. Hanson, A. Connolly Astroparticle Physics 91 (2017) 75-89
ARZ2019: semi MC time domain model from Alvarez-Muñiz, J., Romero-Wolf, A., & Zas, E. (2011). Practical and accurate calculations of Askaryan radiation. Physical Review D - Particles, Fields, Gravitation and Cosmology, 84(10). https://doi.org/10.1103/PhysRevD.84.103003
ARZ2020: semi MC time domain model updated version of ARZ2019 with parameters taken from J. Alvarez-Muñiz, P.M. Hansen, A. Romero-Wolf and E. Zas, Askaryan radiation from neutrino-induced showers in ice, Phys. Rev. D 101 (2020) 083005. https://doi.org/10.1103/PhysRevD.101.083005

interp_factor: float or None

controls the interpolation of the charge-excess profiles in the ARZ model

interp_Factor2: float or None

controls the second interpolation of the charge-excess profiles in the ARZ model

same_shower: bool (default False)

controls the random behviour of picking a shower from the library in the ARZ model, see description there for more details

seed: None or int

the random seed for the Askaryan modules

full_output: bool (default False)

if True, askaryan modules can return additional output

Returns:

time trace: array: the amplitudes for each time bin
additional information: dict: only available if full_output enabled

NuRadioMC.SignalGen.askaryan.get_frequency_spectrum(energy, theta, N, dt, shower_type, n_index, R, model, full_output=False, **kwargs)[source]

returns the complex amplitudes of the frequency spectrum of the neutrino radio signal