bremsstrahlung_thin_target#
- sunkit_spex.emission.bremsstrahlung_thin_target(photon_energies, p, eebrk, q, eelow, eehigh, efd=True, integrator=None)[source]#
Computes the thin-target bremsstrahlung x-ray/gamma-ray spectrum from an isotropic electron distribution function provided in
broken_powerlaw
. The units of the computed flux is photons per second per keV per square centimeter.The electron flux distribution function is a double power law in electron energy with a low-energy cutoff and a high-energy cutoff.
- Parameters:
photon_energies (
numpy.array
) – Array of photon energies to evaluate flux atp (
float
) – Slope below the break energyeebrk (
float
) – Break energyq (
float
) – Slope above the break energyeelow (
float
) – Low energy electron cut offeehigh (
float
) – High energy electron cut offefd (
bool
) – True (default) - input electron distribution is electron flux density distribution (unit electrons cm^-2 s^-1 keV^-1), False - input electron distribution is electron density distribution. (unit electrons cm^-3 keV^-1), This input is not used in the main routine, but is passed to brm2_dmlin and Brm2_Fthinintegrator (callable) – A Python function or method to integrate must support vector limits and match signture
fun(x, a, b, n, *args, **kwargs)
- Returns:
flux – Multiplying the output of Brm2_ThinTarget by a0 gives an array of photon fluxes in photons s^-1 keV^-1 cm^-2, corresponding to the photon energies in the input array eph. The detector is assumed to be 1 AU rom the source. The coefficient a0 is calculated as a0 = nth * V * nnth, where nth: plasma density; cm^-3) V: volume of source; cm^3) nnth: Integrated nonthermal electron flux density (cm^-2 s^-1), if efd = True, or Integrated electron number density (cm^-3), if efd = False
- Return type:
Notes
If you want to plot the derivative of the flux, or the spectral index of the photon spectrum as a function of photon energy, you should set RERR to 1.d-6, because it is more sensitive to RERR than the flux.
Adapted from SSW Brm2_ThinTarget