Pulsar¶
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class
gammapy.astro.source.Pulsar(P_0=<Quantity 0.1 s>, logB=10, n=3, I=<Quantity 1e+45 cm2 g>, R=<Quantity 1000000.0 cm>, age=None, L_0=None, morphology='Delta2D')[source]¶ Bases:
gammapy.astro.source.SimplePulsarMagnetic dipole spin-down pulsar model.
Reference: http://www.cv.nrao.edu/course/astr534/Pulsars.html
Parameters: P_0 : float
Period at birth
logB : float
Logarithm of the magnetic field, which is constant
n : float
Spin-down braking index
I : float
Moment of inertia
R : float
Radius
Methods Summary
energy_integrated([t])Total released energy at age t. luminosity_spindown([t])Spin down luminosity at age t. luminosity_tev([t, fraction])Gamma-ray luminosity assumed to be a certain fraction of the spin-down luminosity. magnetic_field([t])Magnetic field strength at the polar cap. period([t])Period at age t. period_dot([t])Period derivative at age t. tau([t])Characteristic age at real age t. Methods Documentation
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energy_integrated(t=None)[source]¶ Total released energy at age t.
Time-integrated spin-down luminosity since birth.
Parameters: t :
QuantityTime after birth of the pulsar.
Notes
The time integrated energy is given by:
\[E(t) = \dot{L}_0 \tau_0 \frac{t}{t + \tau_0}\]
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luminosity_spindown(t=None)[source]¶ Spin down luminosity at age t.
Parameters: t :
QuantityTime after birth of the pulsar.
Notes
The spin-down luminosity is given by:
\[\dot{L}(t) = \dot{L}_0 \left(1 + \frac{t}{\tau_0}\right)^{\frac{n + 1}{n - 1}}\]
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luminosity_tev(t=None, fraction=0.1)[source]¶ Gamma-ray luminosity assumed to be a certain fraction of the spin-down luminosity.
Parameters: t :
QuantityTime after birth of the pulsar.
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magnetic_field(t=None)[source]¶ Magnetic field strength at the polar cap. Assumed to be constant.
Notes
The magnetic field is given by:
\[B = 3.2\cdot 10^{19} (P\dot{P})^{1/2} [\textnormal(Gauss)]\]
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period(t=None)[source]¶ Period at age t.
Parameters: t :
QuantityTime after birth of the pulsar.
Notes
The period is given by:
\[P(t) = P_0\left(1 + \frac{t}{\tau_0}\right)^{\frac{1}{n - 1}}\]
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