TY - JOUR
T1 - Electron-Ion Temperature Ratio in Transrelativistic Unmagnetized Shock Waves
AU - Vanthieghem, Arno
AU - Tsiolis, Vasileios
AU - Fiuza, Frederico
AU - Sekiguchi, Kazuhiro
AU - Spitkovsky, Anatoly
AU - Todo, Yasushi
N1 - Publisher Copyright:
© Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License.
PY - 2024/7/30
Y1 - 2024/7/30
N2 - Weakly magnetized shock waves are paramount to a large diversity of environments, including supernova remnants, blazars, and binary-neutron-star mergers. Understanding the distribution of energy between electrons and ions within these astrophysical shock waves spanning a wide spectrum of velocities is a long-standing challenge. In this study, we present a unified model for the downstream electron temperature within unmagnetized shock waves. Encompassing velocities from Newtonian to relativistic, we probe regimes representative of the gradual deceleration of the forward shock in the late gamma-ray burst afterglow phase, such as GRB 170817A. In our model, heating results from an ambipolar electric field generated by the difference in inertia between electrons and ions, coupled with rapid electron scattering in the decelerating turbulence. Our findings demonstrate that the electron temperature consistently represents 10% of the incoming ion kinetic energy in the shock front frame over the full range of shock velocities.
AB - Weakly magnetized shock waves are paramount to a large diversity of environments, including supernova remnants, blazars, and binary-neutron-star mergers. Understanding the distribution of energy between electrons and ions within these astrophysical shock waves spanning a wide spectrum of velocities is a long-standing challenge. In this study, we present a unified model for the downstream electron temperature within unmagnetized shock waves. Encompassing velocities from Newtonian to relativistic, we probe regimes representative of the gradual deceleration of the forward shock in the late gamma-ray burst afterglow phase, such as GRB 170817A. In our model, heating results from an ambipolar electric field generated by the difference in inertia between electrons and ions, coupled with rapid electron scattering in the decelerating turbulence. Our findings demonstrate that the electron temperature consistently represents 10% of the incoming ion kinetic energy in the shock front frame over the full range of shock velocities.
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M3 - Conference article
AN - SCOPUS:85200600666
SN - 1824-8039
VL - 461
JO - Proceedings of Science
JF - Proceedings of Science
M1 - 011
T2 - 8th High Energy Phenomena in Relativistic Outflows, HEPRO 2023
Y2 - 23 October 2023 through 26 October 2023
ER -