Functions to compute the emissivity due to synchrotron and Inverse compton processes from isotropic radiation source of Cosmic Microwave Background (CMB) photons for each particle based on its spectral dustribution.
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void | IC_SingleElectronPower (double, double, double *) |
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void | IC_ComputeEmissivity_Petruk (Particle *, double, double *) |
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double | Sync_GetKz (double, void *) |
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void | Sync_GenerateFxAndGx (double, double *, double *) |
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void | GetCrossProduct (double *, double *, double *) |
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void | Sync_PolarisationAngle (double *, double *, double *, double *, double *, double *, double *) |
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int | GetNearestIndex (double, double *, int) |
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void | Particles_LP_Sync_Emissivity (Particle *pl, double freq_GHz, double ThObs, double *JnuSync, double *StkQ, double *StkU) |
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void | Particles_LP_IC_Emissivity (Particle *pl, double freq_GHz, double ThObs, double *JnuIC) |
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◆ GetCrossProduct()
void GetCrossProduct |
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double * |
a, |
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double * |
b, |
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double * |
acrb |
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Function to compute the cross product of two vectors a and b.
- Parameters
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[in] | a | Input Vector a |
[in] | b | Input Vector a |
[out] | acrb | Output Vector that has the cross product a x b |
◆ GetNearestIndex()
int GetNearestIndex |
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double |
value, |
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double * |
x, |
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int |
len |
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Computes the index of the nearest neighbour in a 1D array.
- Parameters
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[in] | value | The input value whose nearest index is sought. |
[in] | x | 1D Array of from which the index is to be obtained. |
[in] | len | Length of the Input array. |
- Returns
- An integer which is the index of the Nearest point.
◆ IC_ComputeEmissivity_Petruk()
void IC_ComputeEmissivity_Petruk |
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Particle * |
pl, |
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double |
freq_GHz, |
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double * |
JnuIC |
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Estimates the power per volume per energy emitted by an ensemble of electron N(E) with Isotropic radiation field of CMB photons. This assumes that the flow is non-relativistic and can be typically used to estimate IC Power from Supernovae.
Multiplication with a factor of h/(4*pi) estimates emissivity JnuIC in units of ergs/s.Hz.cm^3.str for the MHD module.
- Parameters
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[in] | pl | Pointer to the Particle Structure. |
[in] | freq_GHz | Observed frequency of InverseCompton radiation in GHz. |
[out] | JnuIC | Total InverseCompton emissivity at the prescribed frequency |
◆ IC_SingleElectronPower()
void IC_SingleElectronPower |
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double |
SpecE, |
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double |
freq_GHz, |
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double * |
PowSE |
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Estimates the power emitted by single electron at the Observed Frequency (user-defined) as it interacts with Isotropic radiation field of CMB photons. This assumes that the flow is non-relativistic. Typically used to estimate IC Power from Supernovae. Approximations in the Thompson's limit used here are adopted from Petruk, A & A, Vol. 499, 2009 [Eqs. 14 and 33]
- Parameters
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[in] | SpecE | Electron energy in cgs units. |
[in] | freq_GHz | Observed frequency of synchrotron radiation in GHz. |
[out] | PowSE | Power radiatied due to Single Electron (Nonrelativistic Fliud) |
◆ Particles_LP_IC_Emissivity()
void Particles_LP_IC_Emissivity |
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Particle * |
pl, |
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double |
freq_GHz, |
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double |
ThObs, |
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double * |
JnuIC |
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Estimates the power emitted by an ensemble of electron N(E) with Isotropic radiation field of CMB photons. For non-relativistic flow approximations in the Thompson's limit are taken from Petruk et. al. 2009, typically used for Supernovae. For the relativistic flow approximations in the Thompson's limit used here are adopted from Dermer et. al. 1995. The relativistic implementation therefore account of beaming of incident CMB photon and also related relativistic effects. The output –> Total InverseCompton emissivity at the prescribed frequency is obtained in units of ergs/(s*cm^3*str)
- Parameters
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[in] | pl | Pointer to the Particle Structure. |
[in] | freq_GHz | Observed frequency of InverseCompton radiation in GHz. |
[in] | ThObs | Line of Sight Angle subtended from the Z axis in degrees. |
[out] | JnuIC | Total InverseCompton emissivity at the prescribed frequency |
◆ Particles_LP_Sync_Emissivity()
void Particles_LP_Sync_Emissivity |
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Particle * |
pl, |
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double |
freq_GHz, |
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double |
ThObs, |
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double * |
JnuSync, |
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double * |
StkQ, |
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double * |
StkU |
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Routine that computes the total synchrotrn emissivity and polarised Stoke Parameters for a given observed frequency and line of sight angle. The output is obtained in cgs units : ergs/(s*cm^3*Hz*str)
- Parameters
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[in] | pl | Pointer to the Particle Structure. |
[in] | freq_GHz | Observed frequency of synchrotron radiation in GHz. |
[in] | ThObs | Line of Sight Angle subtended from the Z axis in degrees. |
[out] | JnuSync | Total synchrotron emissivity at the prescribed frequency |
[out] | StkQ | Stoke Q Value from Linear Polarised Synchrotron emission. |
[out] | StkU | Stoke U Value from Linear Polarised Synchrotron emission. |
◆ Sync_GenerateFxAndGx()
void Sync_GenerateFxAndGx |
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double |
x, |
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double * |
FxIntp, |
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double * |
GxIntp |
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This routine generates the 1D array of F(x) = Int(K(5/3, z)dz) and G(x) = Int(K(2/3,z)dz) on the first call. These functions are required to compute synchrotron emissivity
- Parameters
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[in] | x | Dimensionless electron energy |
[out] | FxIntp | Interpolated value of F(x)/x |
[out] | GxIntp | Interpolated value of G(x)/x |
◆ Sync_GetKz()
double Sync_GetKz |
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double |
t, |
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void * |
Fx_p |
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This routine computes the value of Modified Bessel Function K_(5/3)(t) using its integral form [Eilek, 1996 Appendix A]. This required to estimate the synchrotron emissivity of single electron.
- Parameters
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[in] | t | Independent variable t |
[in] | Fx_p | Pointer to the structure to modify parameters. |
- Returns
- Returns of the value of K_(5/3)(t).
◆ Sync_PolarisationAngle()
void Sync_PolarisationAngle |
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double * |
B, |
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double * |
V, |
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double * |
nlos, |
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double * |
Dfact, |
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double * |
csPolAng, |
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double * |
snPolAng, |
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double * |
Bperp |
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Compute angle of polarisation required to compute Stoke Parameters from the total emissivity. Appropriate Relativistic corrections are incoprated following the work by Lyutikov (2203) & Del Zanna (2006)
- Parameters
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[in] | B | Magnetic field vector interpolated on a macro-particles |
[in] | V | Three Velocity vector interpolated on a macro-particles |
[in] | nlos | Line of sight vector. |
[out] | Dfact | Doppler Factor. |
[out] | csPolAng | Cosine of the Polarisation Angle to compute Stoke Parameters |
[out] | snPolAng | Sine of the Polarisation Angle to compute Stoke Parameters |
[out] | snChi | Sine of Angle between the B field and line of sight vector in jet frame. |