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)[source]#

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`(t)	Estimate of the magnetic field inside the PWN.
`radius`(t)	Radius of the PWN at age t.

Methods Documentation

magnetic_field(t)[source]#

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(t)[source]#

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.