Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...21112005s&link_type=abstract
American Astronomical Society, AAS Meeting #211, #120.05; Bulletin of the American Astronomical Society, Vol. 39, p.950
Astronomy and Astrophysics
Astronomy
Scientific paper
The emission of electromagnetic radiation from a superluminal (faster-than-light in vacuo) charged particle was first studied by Sommerfeld in 1904. However, the Special Theory of Relativity was published just a few months later; prevailing scientific opinion then effectively curtailed the research field until Ginzberg and coworkers pointed out in the 1980s that no physical principle forbids emission by extended, massless superluminal sources. A polarization current density (dP/dt see Maxwell's fourth equation) can provide such a source; the individual charged particles creating the polarization do not move faster than the speed of light, and yet it is relatively trivial to make the envelope of the polarization current density to do so. Based on these ideas, we have constructed a laboratory apparatus that demonstrates that polarization currents can be made to move faster than the speed of light in vacuo and that these superluminal distribution patterns emit tightly focused packets of electromagnetic radiation that are fundamentally different from the emissions of previously known terrestrial sources. A remarkable aspect of superluminal radiation sources is that the relation between retarded (source) and reception times need not be one-to-one: multiple or even extended retarded times may contribute to a single instant of reception. We have also carried out numerical calculations of the radiation emitted from superluminal polarization currents. Our initial results strongly suggest that superluminal emission is an important process in the observable universe, occurring, for example, in pulsars. By computing the radiation from a rotating superluminal source (supplied in pulsars by the rotating intense magnetic fields from the spinning core), we have been able to reproduce the polarization, image structure, position angles, and apparent radiation temperature of astronomical observations of pulsars, using a single, elegant model with few input parameters and no external assumptions,
Ardavan Arzhang
Ardavan Houshang
Fasel Jean
Perez Martinez M.
Schmidt Albrecht
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