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
- pulsar
Pulsar
Pulsar model instance.
- snr
SNRTrueloveMcKee
SNR model instance
- eta_efloat
Fraction of energy going into electrons.
- eta_Bfloat
Fraction of energy going into magnetic fields.
- age
Quantity
Age of the PWN.
- morphologystr
Morphology model of the PWN
- pulsar
Methods Summary
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
- t
Quantity
Time after birth of the SNR
- t
- 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
- t
Quantity
Time after birth of the SNR
- t