Asymmetric Supernovae, Pulsars, Magnetars, and Gamma-Ray Bursts

We outline the possible physical processes, associated timescales, and energetics that could lead to the production of pulsars, jets, asymmetric supernovae, and weak gamma-ray bursts in routine circumstances and to a magnetar and perhaps stronger gamma-ray burst in more extreme circumstances in the collapse of the bare core of a massive star. The production of a LeBlanc-Wilson MHD jet could provide an asymmetric supernova and result in a weak gamma-ray burst when the jet accelerates down the stellar density gradient of a hydrogen-poor photosphere. The matter-dominated jet would be formed promptly, but requires 5 to 10 s to reach the surface of the progenitor of a Type Ib/c supernova. During this time, the newly-born neutron star could contract, spin up, and wind up field lines or turn on an $\alpha-\Omega$ dynamo. In addition, the light cylinder will contract from a radius large compared to the Alfv\'en radius to a size comparable to that of the neutron star. This will disrupt the structure of any organized dipole field and promote the generation of Large Amplitude Electromagnetic Waves (LAEW). The generation of the LAEW would be delayed by the cooling time of the neutron star $\simeq$ 5 to 10 seconds, but the propagation time is short so the LAEW could arrive at the surface at about the same time as the matter jet. In the density gradient of the star and the matter jet, the intense flux of LAEW could drive shocks, generate pions by proton-proton collision, or create electron/positron pairs depending on the circumstances. The LAEW could influence the dynamics of the explosion and might also tend to flow out the rotation axis to produce a collimated gamma-ray burst.