Fitting Fermi LAT Observations Of Millisecond Pulsars To The Spectrum Of The Emission From A Faster-than-light Source

Details Fitting Fermi LAT Observations Of Millisecond Pulsars To The Spectrum Of The Emission From A Faster-than-light Source Fitting Fermi LAT Observations Of Millisecond Pulsars To The Spectrum Of The Emission From A Faster-than-light Source

May 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21631508s&link_type=abstract

American Astronomical Society, AAS Meeting #216, #315.08; Bulletin of the American Astronomical Society, Vol. 41, p.895

Astronomy and Astrophysics

Astronomy

Scientific paper

In two recent papers we have compared the multiwavelength observations of nine broad-band pulsars with the radiation spectrum generated by a polarization current that rotates faster than light in vacuo and found that this single emission process accounts quantitatively for the spectrum of each pulsar over 16-18 orders of magnitude of frequency. Here we apply the superluminal model to data from millisecond Gamma-ray pulsars detected by the Fermi Large Area Telescope (LAT). In order to describe broadband pulsar data using the superluminal model, the two most important parameters are ω, the pulsar's (known) 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, i.e. Ω = (Ne2/ɛ0me)1/2, where N is the number density of electrons and me is the electron mass. All of the pulsars investigated exhibit one further feature; an enhancement of the emission at higher frequencies. This will occur if the permittivity of the pulsar atmosphere has a second resonant frequency mω, where m is a (large) integer; we attribute this to cyclotron resonance of the electrons in the pulsar's magnetic field. Using the values of Ω and mω from fitting the data for the LAT millisecond pulsars, we have extracted values for N and the magnetic field B at the emitting region and derived some systematic properties of their plasma atmospheres. The results reported here are model-independent in that the only global property of the magnetospheric structure invoked is its quasi-steady time dependence, a property that follows unambiguously from the observational data and implies that a current distribution with a superluminally rotating pattern at a radius r > c/ω is responsible for the unique features of pulsar emission.

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