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X-ray Synchrotron Polarization from Turbulent Plasmas in Supernova Remnants

Published online by Cambridge University Press:  17 October 2017

Matthew G. Baring
Matthew G. Baring*
Affiliation:
Department of Physics and Astronomy - MS 108, Rice University, 6100 Main Street, Houston, Texas 77251-1892, USA email: [email protected]
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Abstract

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As supernova remnants (SNRs) age, they become efficient cosmic ray accelerators at their outer shell shocks. The current paradigm for shock acceleration theory favors turbulent field environs in the proximity of these shocks, turbulence driven by current instabilities involving energetic ions. With the imminent prospect of dedicated X-ray polarimeters becoming a reality, the possibility looms of probing turbulence on scales that couple to the super-TeV electrons that emit X-rays. This paper presents model X-ray polarization signatures from energetic electrons moving in simulated MHD turbulence of varying levels of “chaos.” The emission volumes are finite slabs that represent the active regions of young SNR shells. We find that the turbulent field energy must be quite limited relative to that of the total field in order for the X-ray polarization degree to be as strong as the radio measures obtained in some remnants. Results presented are pertinent to the planned IXPE and XIPE polarimeters.

Keywords

supernova remnantscosmic raysradiation mechanisms: nonthermalpolarizationplasmasturbulence
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S331: Supernova 1987A:30 years later - Cosmic Rays and Nuclei from Supernovae and their aftermaths , February 2017 , pp. 242 - 247
Copyright
Copyright © International Astronomical Union 2017 

References

Bell, A. R. 2005, MNRAS, 358, 181 CrossRefGoogle Scholar
Bykov, A. M., Uvarov, Yu. A., Bloemen, J. B. G. M., et al. 2009, MNRAS, 399, 1119 Google Scholar
Giacalone, J. & Jokipii, J. R. 1999, Astrophys. J., 520, 204 Google Scholar
Long, K. S., Reynolds, S. P., Raymond, J. C., et al. 2003, Astrophys J., 586, 1162 CrossRefGoogle Scholar
Lucek, S. G. & Bell, A. R. 2000, MNRAS, 314, 65 CrossRefGoogle Scholar
Reynolds, S. P. & Gilmore, D. M. 1993, Astronomical J, 106, 272 Google Scholar
Reynoso, E. M., Hughes, J. P., & Moffett, D. A. 2013, Astrophys. J., 145:104 Google Scholar
Rybicki, G. B. & Lightman, A. P. 1979 Radiative Processes in Astrophysics (Wiley, New York)Google Scholar
Soffitta, P., Barcons, X., Bellazzini, R., et al. 2013, Experimental Astronomy, 36, 523 CrossRefGoogle Scholar
Vink, J. & Laming, J. M. 2003, Astrophys. J., 584, 758 Google Scholar
Vladimirov, A., Ellison, D. C., & Bykov, A. 2006, Astrophys. J., 652, 1246 CrossRefGoogle Scholar
Weisskopf, M. C., Baldini, L., Bellazini, R., et al. 2013, in Proc. SPIE, Vol. 8859, UV, X-Ray, and Gamma-Ray Space Instrumentation for Astronomy XVIII, 885908Google Scholar