PWN

class gammapy.astro.source.PWN(pulsar=<gammapy.astro.source.pulsar.Pulsar object>, snr=<gammapy.astro.source.snr.SNRTrueloveMcKee object>, eta_e=0.999, eta_B=0.001, morphology='Gaussian2D', age=None)

Bases: object

Simple pulsar wind nebula (PWN) evolution model.

Parameters

pulsarPulsar

Pulsar model instance.

snrSNRTrueloveMcKee

SNR model instance

eta_efloat

Fraction of energy going into electrons.

eta_Bfloat

Fraction of energy going into magnetic fields.

ageQuantity

Age of the PWN.

morphologystr

Morphology model of the PWN

Methods Summary

magnetic_field(self, t)	Estimate of the magnetic field inside the PWN.
radius(self, t)	Radius of the PWN at age t.

Methods Documentation

magnetic_field(self, t)

Estimate of the magnetic field inside the PWN.

By assuming that a certain fraction of the spin down energy is converted to magnetic field energy an estimation of the magnetic field can be derived.

Parameters

tQuantity

Time after birth of the SNR

radius(self, t)

Radius of the PWN at age t.

During the free expansion phase the radius of the PWN evolves like:

\[R_{PWN}(t) = 1.44 \left(\frac{E_{SN}^3\dot{E}_0^2} {M_{ej}^5}\right)^{1/10}t^{6/5} \text{pc}\]

After the collision with the reverse shock of the SNR, the radius is assumed to be constant (See radius_reverse_shock).

Reference: https://ui.adsabs.harvard.edu/abs/2006ARA%26A..44…17G (Formula 8).

Parameters

tQuantity

Time after birth of the SNR