Pulsars in the High Energy and Early Universe

The mechanism of polarization currents excited supraluminally (updated faster than c) by rotating neutron star magnetospheres (SLIP) can be used to explain the means by which supernova progenitors are disrupted, including the details of SN 1987A. At radii of a few times that of the light cylinder the effect helps to lift material way from the core. At much greater radii, the paths from current-containing annuli clear the stellar core on the way to the poles, where the concentration of the effects results in highly collimated pulsar-driven jets with velocities in excess of 0.95c, and element transmutation via the r-process. SLIP also accounts for the anomalous dimming of SNe Ia at cosmological distances, jets from Sco X-1 and SS 433, the lack/presence of pulsations from the high/low luminosity low mass X-ray binaries, long/short gamma-ray bursts, and predicts that their afterglows are the pulsed optical-/near-infrared emission associated with the pulsars. Pulsar-driven jets from the SNe of the first stars may allow galaxies to form without the need for dark matter. SLIP may also account for the TeV e+/e- results from PAMELA and ATIC, the WMAP "haze"/Fermi "bubbles", and the spectrum of the nine Fermi-LAT pulsars with radio observations, over 16-18 orders of magnitude of frequency with minimal adjustable parameters. With parameters extracted from the broadband fits, we have calculated values for the number density of electrons and the magnetic field, B, at the emitting region and derived some systematic properties of these pulsars' plasma atmospheres.