Modeling the broadband persistent emission of magnetars
arXiv:1008.1537 · doi:10.1016/j.asr.2010.08.003
Abstract
In this paper, we discuss our first attempts to model the broadband persistent emission of magnetars within a self consistent, physical scenario. We present the predictions of a synthetic model that we calculated with a new Monte Carlo 3-D radiative code. The basic idea is that soft thermal photons (e.g. emitted by the star surface) can experience resonant cyclotron upscattering by a population of relativistic electrons threated in the twisted magnetosphere. Our code is specifically tailored to work in the ultra-magnetized regime; polarization and QED effects are consistently accounted for, as well different configurations for the magnetosphere. We discuss the predicted spectral properties in the 0.1-1000 keV range, the polarization properties, and we present the model application to a sample of magnetars soft X-ray spectra.
14 pages, 7 figures, to be published in Advances in Space Research. Proceedings of the conference "Frontieres of Space Astrophysics, Neutron Stars & Gamma Ray Bursts", Cairo/Alexandria, 30 March- 4 April 2009
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- Probing magnetar emission mechanisms with spectropolarimetry
- The INTEGRAL view of the pulsating hard X-ray sky: from accreting and transitional millisecond pulsars to rotation-powered pulsars and magnetars
- Spectral Modification of Magnetar Flares by Resonant Cyclotron Scattering
- Polarized Radiation Transfer in Neutron Star Surface Layers
- Axion Constraints from Quiescent Soft Gamma-ray Emission from Magnetars
- Persistent Emission Properties of SGR J1935+2154 During Its 2020 Active Episode
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