Abstract
Abstract
Magnetic reconnection is often invoked as a source of high-energy particles, and in relativistic astrophysical systems it is regarded as a prime candidate for powering fast and bright flares. We present a novel analytical model—supported and benchmarked with large-scale three-dimensional kinetic particle-in-cell simulations in electron–positron plasmas—that elucidates the physics governing the generation of power-law energy spectra in relativistic reconnection. Particles with Lorentz factor γ ≳ 3σ (here, σ is the magnetization) gain most of their energy in the inflow region, while meandering between the two sides of the reconnection layer. Their acceleration time is
t
acc
∼
γ
η
rec
−
1
ω
c
−
1
≃
20
γ
ω
c
−
1
, where η
rec ≃ 0.06 is the inflow speed in units of the speed of light and ω
c = eB
0/mc is the gyrofrequency in the upstream magnetic field. They leave the region of active energization after t
esc, when they get captured by one of the outflowing flux ropes of reconnected plasma. We directly measure t
esc in our simulations and find that t
esc ∼ t
acc for σ ≳ few. This leads to a universal (i.e., σ-independent) power-law spectrum
dN
free
/
d
γ
∝
γ
−
1
for the particles undergoing active acceleration, and
dN
/
d
γ
∝
γ
−
2
for the overall particle population. Our results help to shed light on the ubiquitous presence of power-law particle and photon spectra in astrophysical nonthermal sources.
Funder
National Science Foundation
Publisher
American Astronomical Society
Subject
Space and Planetary Science,Astronomy and Astrophysics
Cited by
7 articles.
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