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GRBICompton Class Reference

ICompton emission process. More...

#include <GRBICompton.h>

Inheritance diagram for GRBICompton::

List of all members.

Public Methods
	GRBICompton ()
	GRBICompton (SpectObj spectrumObj)
	~GRBICompton ()
void	load (const GRBShock *Shock, const double time=0.0, const double angle=0.0, const double distance_to_source=0.0)
void	load (const double time=0.0, const double angle=0.0, const double distance_to_source=0.0, const double GAMMAF=500., const double B=1.0e+6, const double N0=1.0e+50, const double gamma_min=1., const double gamma_max=1.0e+10, const double Vol=1.0e+40, const double dr=1.0e+10)
double	InverseComptonFunction (double g0, double e0, double energy)
	Inverse Compton Function. More...

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Detailed Description

ICompton emission process.

This class compute the Inverse Compton scattering emission. This process is represented by The energy of the incident electron ( ) is greater then the energy of the incident photon ( ). The scattered electron give part of its energy to the photon. The energy of the scattered photon roughly increases by a factor , unless the Klein Nishina limit is reached.

The easiest way to compute the IC emission is to adopt a power law assumption, where only a part of the entire population of electrons is used. In this class either the power law approximation and the full integration on the electron distribution are used.

Author:

Nicola Omodei nicola.omodei@pi.infn.it , Johann Cohen-Tanugi johann.cohen@pi.infn.it

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Member Function Documentation

double GRBICompton::InverseComptonFunction (  double    g0, double    e0, double    energy )

Inverse Compton Function. This Function represents the probability to obtain a photon photon with energy energy from the scattering of an electron of energy and a photon with energy . Parameters: energy, final  energy of the photon after the scattering e0  initial energy of the photon g0  Lorentz factor of the incident electron This function has been derived by Blumenthal and Gould (1970) To obtain the Inverse vompton emissivity we have to integrate over the distribution of the seed photon and over the electron distribution.

void GRBICompton::load (  const double    time = 0.0, const double    angle = 0.0, const double    distance_to_source = 0.0, const double    GAMMAF = 500., const double    B = 1.0e+6, const double    N0 = 1.0e+50, const double    gamma_min = 1., const double    gamma_max = 1.0e+10, const double    Vol = 1.0e+40, const double    dr = 1.0e+10 )

General Interface for computing the IC spectrum at a certain

void GRBICompton::load (  const GRBShock *    Shock, const double    time = 0.0, const double    angle = 0.0, const double    distance_to_source = 0.0 )

Given a Shock compute the spectrum at a certain time /param *Shock contains all the information to compute the emission /param time is the rtime to compute the spectrum /param angle is needed to compute the observed spectrum /param distance_to_source is the distance of the source (in cm)

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The documentation for this class was generated from the following file:

• GRBICompton.h

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