Non-thermal particle acceleration in collisionless relativistic electron–proton reconnection
Abstract
Magnetic reconnection in relativistic collisionless plasmas can accelerate particles and power high-energy emission in various astrophysical systems. Whereas most previous studies focused on relativistic reconnection in pair plasmas, less attention has been paid to electron–ion plasma reconnection, expected in black hole accretion flows and relativistic jets. In this paper, we report a comprehensive particle-in-cell numerical investigation of reconnection in an electron–ion plasma, spanning a wide range of ambient ion magnetizations σi, from the semirelativistic regime (ultrarelativistic electrons but non-relativistic ions, 10-3 ≪ σi ≪ 1) to the fully relativistic regime (both species are ultrarelativistic, σi ≫ 1). We investigate how the reconnection rate, electron and ion plasma flows, electric and magnetic field structures, electron/ion energy partitioning, and non-thermal particle acceleration depend on σi. Our key findings are: (1) the reconnection rate is about 0.1 of the Alfvénic rate across all regimes; (2) electrons can form concentrated moderately relativistic outflows even in the semirelativistic, small-σi regime; (3) while the released magnetic energy is partitioned equally between electrons and ions in the ultrarelativistic limit, the electron energy fraction declines gradually with decreased σi and asymptotes to about 0.25 in the semirelativistic regime; and (4) reconnection leads to efficient non-thermal electron acceleration withmore »
- Authors:
-
- Univ. of Colorado, Boulder, CO (United States)
- Univ. of Colorado, Boulder, CO (United States); Institute for Advanced Study, Princeton, NJ (United States)
- University of Colorado and National Institute of Standards and Technology, Boulder, CO (United States)
- Université Grenoble Alpes, CNRS (France)
- Polish Academy of Sciences, Warsaw (Poland)
- Publication Date:
- Research Org.:
- Univ. of Colorado, Boulder, CO (United States); Univ. of New Hampshire, Durham, NH (United States); Argonne National Laboratory (ANL), Argonne, IL (United States)
- Sponsoring Org.:
- USDOE Office of Science (SC)
- OSTI Identifier:
- 1512962
- Grant/Contract Number:
- SC0008409; SC0008655; AC02-06CH11357
- Resource Type:
- Accepted Manuscript
- Journal Name:
- Monthly Notices of the Royal Astronomical Society
- Additional Journal Information:
- Journal Volume: 473; Journal Issue: 4; Journal ID: ISSN 0035-8711
- Publisher:
- Royal Astronomical Society
- Country of Publication:
- United States
- Language:
- English
- Subject:
- 43 PARTICLE ACCELERATORS; acceleration of particles; accretion; accretion discs; magnetic reconnection; relativistic processes; BL Lacertae objects: general; X-rays: binaries
Citation Formats
Werner, G. R., Uzdensky, D. A., Begelman, M. C., Cerutti, B., and Nalewajko, K. Non-thermal particle acceleration in collisionless relativistic electron–proton reconnection. United States: N. p., 2017.
Web. doi:10.1093/mnras/stx2530.
Werner, G. R., Uzdensky, D. A., Begelman, M. C., Cerutti, B., & Nalewajko, K. Non-thermal particle acceleration in collisionless relativistic electron–proton reconnection. United States. https://doi.org/10.1093/mnras/stx2530
Werner, G. R., Uzdensky, D. A., Begelman, M. C., Cerutti, B., and Nalewajko, K. Thu .
"Non-thermal particle acceleration in collisionless relativistic electron–proton reconnection". United States. https://doi.org/10.1093/mnras/stx2530. https://www.osti.gov/servlets/purl/1512962.
@article{osti_1512962,
title = {Non-thermal particle acceleration in collisionless relativistic electron–proton reconnection},
author = {Werner, G. R. and Uzdensky, D. A. and Begelman, M. C. and Cerutti, B. and Nalewajko, K.},
abstractNote = {Magnetic reconnection in relativistic collisionless plasmas can accelerate particles and power high-energy emission in various astrophysical systems. Whereas most previous studies focused on relativistic reconnection in pair plasmas, less attention has been paid to electron–ion plasma reconnection, expected in black hole accretion flows and relativistic jets. In this paper, we report a comprehensive particle-in-cell numerical investigation of reconnection in an electron–ion plasma, spanning a wide range of ambient ion magnetizations σi, from the semirelativistic regime (ultrarelativistic electrons but non-relativistic ions, 10-3 ≪ σi ≪ 1) to the fully relativistic regime (both species are ultrarelativistic, σi ≫ 1). We investigate how the reconnection rate, electron and ion plasma flows, electric and magnetic field structures, electron/ion energy partitioning, and non-thermal particle acceleration depend on σi. Our key findings are: (1) the reconnection rate is about 0.1 of the Alfvénic rate across all regimes; (2) electrons can form concentrated moderately relativistic outflows even in the semirelativistic, small-σi regime; (3) while the released magnetic energy is partitioned equally between electrons and ions in the ultrarelativistic limit, the electron energy fraction declines gradually with decreased σi and asymptotes to about 0.25 in the semirelativistic regime; and (4) reconnection leads to efficient non-thermal electron acceleration with a σi-dependent power-law index, p(σi)≃const + 0.7σi-1/2. Finally, these findings are important for understanding black hole systems and lend support to semirelativistic reconnection models for powering non-thermal emission in blazar jets, offering a natural explanation for the spectral indices observed in these systems.},
doi = {10.1093/mnras/stx2530},
journal = {Monthly Notices of the Royal Astronomical Society},
number = 4,
volume = 473,
place = {United States},
year = {Thu Sep 28 00:00:00 EDT 2017},
month = {Thu Sep 28 00:00:00 EDT 2017}
}
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Figures / Tables:
Figure 1: The dependence of cold and hot magnetization parameters on $σ$$i$ (the ‘cold’ $σ$ with respect to background ions). Circles mark the values of $σ$$i$ for simulations described in this paper.
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