PWN¶
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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_e : float
Fraction of energy going into electrons.
eta_B : float
Fraction of energy going into magnetic fields.
age :
Quantity
Age of the PWN.
morphology : str
Morphology model of the PWN
Methods Summary
luminosity_tev
([t, fraction])Simple luminosity evolution model. magnetic_field
([t])Estimate of the magnetic field inside the PWN. radius
([t])Radius of the PWN at age t. Methods Documentation
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luminosity_tev
(t=None, fraction=0.1)[source]¶ Simple luminosity evolution model.
Assumes that the luminosity is just a fraction of the total energy content of the pulsar. No cooling is considered and therefore the estimate is very bad.
Parameters: t :
Quantity
Time after birth of the SNR.
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magnetic_field
(t=None)[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.
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radius
(t=None)[source]¶ Radius of the PWN at age t.
Reference: http://adsabs.harvard.edu/abs/2006ARA%26A..44...17G (Formula 8).
Parameters: t :
Quantity
Time after birth of the SNR.
Notes
During the free expansion phase the radius of the PWN evolves like:
\[R_{PWN}(t) = 1.44\text{pc}\left(\frac{E_{SN}^3\dot{E}_0^2} {M_{ej}^5}\right)^{1/10}t^{6/5}\]After the collision with the reverse shock of the SNR, the radius is assumed to be constant (See
radius_reverse_shock
)
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