Hard X-ray Emission by Resonant Compton Upscattering in Magnetars

Details Hard X-ray Emission by Resonant Compton Upscattering in Magnetars Hard X-ray Emission by Resonant Compton Upscattering in Magnetars

Jan 2012

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012aas...21922608w&link_type=abstract

American Astronomical Society, AAS Meeting #219, #226.08

Astronomy and Astrophysics

Astronomy

Scientific paper

For inner magnetospheric models of hard X-ray and gamma-ray emission in high-field pulsars and magnetars, resonant Compton upscattering is anticipated to be the most efficient process for generating continuum radiation. For magnetars, this is due in part to the proximity of a hot soft photon bath from the stellar surface. Moreover, the scattering cross section becomes resonant at the cyclotron frequency, exceeding the classical Thomson value by over two orders of magnitude and thereby enhancing the efficiency of continuum production and the cooling of relativistic electrons. We present angle-dependent hard X-ray upscattering model spectra for uncooled monoenergetic relativistic electrons injected in inner regions of pulsar magnetospheres. These spectra are integrated over closed field lines and obtained for different observing perspectives. Electron cooling rates for resonant Compton interactions are also presented, in preparation for future radiation-reaction limited acceleration and emission models of non-thermal magnetar X-rays. Our research employs a new Sokolov and Ternov (ST) formulation of the QED Compton scattering cross section in strong magnetic fields. Such an ST formalism is formally correct for treating spin-dependent effects that are important in the cyclotron resonance, and has not been addressed before in the context of Compton upscattering models of magnetar hard X-ray tail emission.

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