Crab pulsar radiation Regarding the radiation from the Crab pulsar and nebula, some reading leads me to the following conclusions.


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*The rotation energy of the neutron star is the source of the non-thermal electromagnetic radiation from the neutron star and the nebula. The rotation also supplies the energy for the electrons in the pulsar wind. The magnetic field of the neutron star acts as an intermediary.

*Most of the non-thermal electromagnetic energy is emitted by the neutron star as magnetic dipole radiation at the spin frequency of the pulsar (Crab: $\lambda=10^7\text{ m}$).

*A small fraction of the non-thermal electromagnetic energy is emitted by the surrounding nebula as radio waves ($\lambda\ll10^7\text{m}$), visible light, röntgen and gamma radiation. This fraction may be curvature or synchrotron radiation or result from inverse compton scattering.

*The surface of the neutron star produces blackbody radiation at a temperature of about 2 MK. The source of this energy is thermal.

*A young pulsar like the Crab also looses a lot of thermal energy by neutino emission (URCA process, neutrino bremsstrahlung).


Are these conclusions more or less correct?
 A: 


*Most of the non-thermal electromagnetic energy is emitted by the neutron star as magnetic dipole radiation at the spin frequency of the pulsar (Crab: λ=107 m).


No, this is not correct. The vast majority of electromagnetic radiation is produced only after the Poyting dominated cold relativistic wind passes through the termination shock. Here is where the plasma is shock-heated and enters the nebula bubble.
Even the jets (and their radiative emission) are directly caused by this post shock flow. Almost all of the radition produced by the Crab is in one way or the other a result of shock heating via the termination shock. All of the main radiative features of the nebula can be modeled with astounding accuracy via the post shock flow alone.
I'd say your other points are about right (obviously omitting lots of intricate details). I hope this helps.

Edit. If you would like to read a paper that covers some aspect of what I have said above, see  MNRAS paper [Observations of "wisps" in magnetohydrodynamic simulations of the Crab Nebula] (https://arxiv.org/abs/0907.3647).
