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arxiv: 2301.07397 · v2 · pith:HHWMMTIYnew · submitted 2023-01-18 · 🌌 astro-ph.HE

X-ray polarimetry reveals the magnetic field topology on sub-parsec scales in Tycho's supernova remnant

Riccardo Ferrazzoli , Patrick Slane , Dmitry Prokhorov , Ping Zhou , Jacco Vink , Niccol\`o Bucciantini , Enrico Costa , Niccol\`o Di Lalla
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Alessandro Di Marco Paolo Soffitta Martin C. Weisskopf Kazunori Asakura Luca Baldini Jeremy Heyl Philip E. Kaaret Fr\'ed\'eric Marin Tsunefumi Mizuno C.-Y. Ng Melissa Pesce-Rollins Stefano Silvestri Carmelo Sgr\`o Douglas A. Swartz Toru Tamagawa Yi-Jung Yang Iv\'an Agudo Lucio A. Antonelli Matteo Bachetti Wayne H. Baumgartner Ronaldo Bellazzini Stefano Bianchi Stephen D. Bongiorno Raffaella Bonino Alessandro Brez Fiamma Capitanio Simone Castellano Elisabetta Cavazzuti Chien-Ting Chen Stefano Ciprini Alessandra De Rosa Ettore Del Monte Laura Di Gesu Immacolata Donnarumma Victor Doroshenko Michal Dov\v{c}iak Steven R. Ehlert Teruaki Enoto Yuri Evangelista Sergio Fabiani Javier A. Garcia Shuichi Gunji Kiyoshi Hayashida Wataru Iwakiri Svetlana G. Jorstad Fabian Kislat Vladimir Karas Takao Kitaguchi Jeffery J. Kolodziejczak Henric Krawczynski Fabio La Monaca Luca Latronico Ioannis Liodakis Simone Maldera Alberto Manfreda Andrea Marinucci Alan P. Marscher Herman L. Marshall Giorgio Matt Ikuyuki Mitsuishi Fabio Muleri Michela Negro Stephen L. O'Dell Nicola Omodei Chiara Oppedisano Alessandro Papitto George G. Pavlov Abel L. Peirson Matteo Perri Pierre-Olivier Petrucci Maura Pilia Andrea Possenti Juri Poutanen Simonetta Puccetti Brian D. Ramsey John Rankin Ajay Ratheesh Oliver Roberts Roger W. Romani Gloria Spandre Fabrizio Tavecchio Roberto Taverna Yuzuru Tawara Allyn F. Tennant Nicholas E. Thomas Francesco Tombesi Alessio Trois Sergey S. Tsygankov Roberto Turolla Kinwah Wu Fei Xie Silvia Zane
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classification 🌌 astro-ph.HE
keywords magnetic-fieldpolarizationx-rayturbulenceaccelerationdegreeremnantshock
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Supernova remnants are commonly considered to produce most of the Galactic cosmic rays via diffusive shock acceleration. However, many questions about the physical conditions at shock fronts, such as the magnetic-field morphology close to the particle acceleration sites, remain open. Here we report the detection of a localized polarization signal from some synchrotron X-ray emitting regions of Tycho's supernova remnant made by the Imaging X-ray Polarimetry Explorer. The derived polarization degree of the X-ray synchrotron emission is 9+/-2% averaged over the whole remnant, and 12+/-2% at the rim, higher than the 7-8% polarization value observed in the radio band. In the west region the polarization degree is 23+/-4%. The X-ray polarization degree in Tycho is higher than for Cassiopeia A, suggesting a more ordered magnetic-field or a larger maximum turbulence scale. The measured tangential polarization direction corresponds to a radial magnetic field, and is consistent with that observed in the radio band. These results are compatible with the expectation of turbulence produced by an anisotropic cascade of a radial magnetic-field near the shock, where we derive a magnetic-field amplification factor of 3.4+/-0.3. The fact that this value is significantly smaller than those expected from acceleration models is indicative of highly anisotropic magnetic-field turbulence, or that the emitting electrons either favor regions of lower turbulence, or accumulate close to where the magnetic-field orientation is preferentially radially oriented due to hydrodynamical instabilities.

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