Microphysics of Relativistic Collisionless Electron-ion-positron Shocks
Abstract
Abstract We perform particle-in-cell simulations to elucidate the microphysics of relativistic weakly magnetized shocks loaded with electron-positron pairs. Various external magnetizations σ ≲ 10 −4 and pair-loading factors Z ± ≲ 10 are studied, where Z ± is the number of loaded electrons and positrons per ion. We find the following: (1) The shock becomes mediated by the ion Larmor gyration in the mean field when σ exceeds a critical value σ L that decreases with Z ± . At σ ≲ σ L the shock is mediated by particle scattering in the self-generated microturbulent fields, the strength and scale of which decrease with Z ± , leading to lower σ L . (2) The energy fraction carried by the post-shock pairs is robustly in the range between 20% and 50% of the upstream ion energy. The mean energy per post-shock electron scales as . (3) Pair loading suppresses nonthermal ion acceleration at magnetizations as low as σ ≈ 5 × 10 −6 . The ions then become essentially thermal with mean energy , while electrons form a nonthermal tail, extending from to . When σ = 0, particle acceleration is enhanced by the formation of intense magnetic cavities that populate the precursor during the late stages of shock evolution. Here, the maximum energy of the nonthermal ions and electrons keeps growing over the duration of the simulation. Alongside the simulations, we develop theoretical estimates consistent with the numerical results. Our findings have important implications for models of early gamma-ray burst afterglows.
- Authors:
- Publication Date:
- Research Org.:
- Oak Ridge Institute for Science and Education (ORISE), Oak Ridge, TN (United States)
- Sponsoring Org.:
- USDOE Office of Science (SC)
- OSTI Identifier:
- 2281424
- Alternate Identifier(s):
- OSTI ID: 1983276
- Grant/Contract Number:
- SC0014664
- Resource Type:
- Published Article
- Journal Name:
- The Astrophysical Journal
- Additional Journal Information:
- Journal Name: The Astrophysical Journal Journal Volume: 933 Journal Issue: 1; Journal ID: ISSN 0004-637X
- Publisher:
- American Astronomical Society
- Country of Publication:
- United States
- Language:
- English
- Subject:
- 79 ASTRONOMY AND ASTROPHYSICS; Astronomy & Astrophysics; High energy astrophysics; Shocks; Non-thermal radiation sources; Plasma astrophysics; Gamma-ray bursts
Citation Formats
Grošelj, Daniel, Sironi, Lorenzo, and Beloborodov, Andrei M. Microphysics of Relativistic Collisionless Electron-ion-positron Shocks. United States: N. p., 2022.
Web. doi:10.3847/1538-4357/ac713e.
Grošelj, Daniel, Sironi, Lorenzo, & Beloborodov, Andrei M. Microphysics of Relativistic Collisionless Electron-ion-positron Shocks. United States. https://doi.org/10.3847/1538-4357/ac713e
Grošelj, Daniel, Sironi, Lorenzo, and Beloborodov, Andrei M. Tue .
"Microphysics of Relativistic Collisionless Electron-ion-positron Shocks". United States. https://doi.org/10.3847/1538-4357/ac713e.
@article{osti_2281424,
title = {Microphysics of Relativistic Collisionless Electron-ion-positron Shocks},
author = {Grošelj, Daniel and Sironi, Lorenzo and Beloborodov, Andrei M.},
abstractNote = {Abstract We perform particle-in-cell simulations to elucidate the microphysics of relativistic weakly magnetized shocks loaded with electron-positron pairs. Various external magnetizations σ ≲ 10 −4 and pair-loading factors Z ± ≲ 10 are studied, where Z ± is the number of loaded electrons and positrons per ion. We find the following: (1) The shock becomes mediated by the ion Larmor gyration in the mean field when σ exceeds a critical value σ L that decreases with Z ± . At σ ≲ σ L the shock is mediated by particle scattering in the self-generated microturbulent fields, the strength and scale of which decrease with Z ± , leading to lower σ L . (2) The energy fraction carried by the post-shock pairs is robustly in the range between 20% and 50% of the upstream ion energy. The mean energy per post-shock electron scales as E ¯ e ∝ Z ± + 1 − 1 . (3) Pair loading suppresses nonthermal ion acceleration at magnetizations as low as σ ≈ 5 × 10 −6 . The ions then become essentially thermal with mean energy E ¯ i , while electrons form a nonthermal tail, extending from E ∼ Z ± + 1 − 1 E ¯ i to E ¯ i . When σ = 0, particle acceleration is enhanced by the formation of intense magnetic cavities that populate the precursor during the late stages of shock evolution. Here, the maximum energy of the nonthermal ions and electrons keeps growing over the duration of the simulation. Alongside the simulations, we develop theoretical estimates consistent with the numerical results. Our findings have important implications for models of early gamma-ray burst afterglows.},
doi = {10.3847/1538-4357/ac713e},
journal = {The Astrophysical Journal},
number = 1,
volume = 933,
place = {United States},
year = {Tue Jul 05 00:00:00 EDT 2022},
month = {Tue Jul 05 00:00:00 EDT 2022}
}
https://doi.org/10.3847/1538-4357/ac713e
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