Other
Scientific paper
May 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21832002s&link_type=abstract
American Astronomical Society, AAS Meeting #218, #320.02; Bulletin of the American Astronomical Society, Vol. 43, 2011
Other
Scientific paper
Recently, we compared multiwavelength observations of nine pulsars with the radiation generated by a polarization current that travels faster than light in a circular orbit, the so-called Superluminal Model for Pulsars (SMP). We found that this single emission process accounts quantitatively for the spectrum of each pulsar over 16-18 orders of magnitude of frequency with minimal adjustable parameters. Here we apply the SMP to observations of gamma-ray emitting pulsars by the Fermi Large Area Telescope (LAT) combined with radio-frequency observations from other instruments.
The SMP invokes emission by superluminal (faster than light) polarization currents. In this context, polarization P results from displacement of positive and negative charges in opposite directions; a polarization current occurs when a polarized region moves or changes with time t. If a polarization current oscillates or accelerates, it will emit electromagnetic radiation, just as a current of electrons does. However, unlike electrons, which possess rest mass and are therefore limited to subluminal speeds, polarization currents are moving patterns that may travel arbitrarily fast.
While the overall form of the fitted spectra is given by the superluminal nature of the source, their fine structure is influenced by the detailed behavior of the pulsar atmosphere. The two most important parameters are ω, the pulsar's rotational frequency, and ω, a resonant frequency of the atmosphere around where the emission occurs. It is natural to ascribe the latter to the plasma frequency. All of the pulsars investigated exhibit one further feature; an enhancement of the emission at higher frequencies, which can be attributed to cyclotron resonance of the electrons in the pulsar's magnetic field. 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.
Ardavan Houshang
Middleditch John
Schmidt Andrea C.
Singleton John
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