<abstract xmlns="http://www.w3.org/1999/xhtml">

We explore the kinetic energy partitions between electrons and ions in the 2-D magnetostatic equilibria called Arnold–Beltrami–Childress (ABC) fields, using particle-in-cell (PIC) numerical simulations. We cover a wider range of ion–electron temperature combinations and get different results compared to previous studies of the Harris-layer-type magnetic reconnection simulations. We find that the initial ion–electron enthalpy ratio is an important indicator. The particle species that dominates the total enthalpy will also dominate the kinetic energy gains and the momentum distribution peaks, but the other species have higher nonthermal energy fractions because both species show similar maximum energies.
</abstract>

We explore the kinetic energy partitions between electrons and ions in the 2-D magnetostatic equilibria called Arnold–Beltrami–Childress (ABC) fields, using particle-in-cell (PIC) numerical simulations. We cover a wider range of ion–electron temperature combinations and get different results compared to previous studies of the Harris-layer-type magnetic reconnection simulations. We find that the initial ion–electron enthalpy ratio is an important indicator. The particle species that dominates the total enthalpy will also dominate the kinetic energy gains and the momentum distribution peaks, but the other species have higher nonthermal energy fractions because both species show similar maximum energies.

<div xmlns="http://www.w3.org/1999/xhtml">
<sec id="j_nuka-2023-0004_s_001">
<div>Introduction</div>
Various astrophysical environments involve extremely rapid and very luminous gamma-ray flares, such as the blazars and the Crab pulsar wind nebula (PWN). Particle acceleration mechanisms are needed to explain how magnetic energy is released and converted to kinetic energy. Currently, magnetic reconnection is one of the very promising candidates (for a review, see references [<a ref-type="bibr" href="#j_nuka-2023-0004_ref_001">1</a>, <a ref-type="bibr" href="#j_nuka-2023-0004_ref_002">2</a>]).
The essential condition for triggering magnetic reconnection includes oppositely directed magnetic fields and a very thin current sheet that can be produced by certain plasma instabilities. The traditional magnetic field configuration is the Harris-layer-type kinetic equilibrium [<a ref-type="bibr" href="#j_nuka-2023-0004_ref_003">3</a>], in which the kinetic-scale current layer limits the outflow (reconnection rate) to the order of <italic>∂</italic>(0.1); hence, the magnetic dissipation efficiency is also limited. In order to understand the rapid and efficient conversion of electromagnetic energy into radiation, the Arnold–Beltrami–Childress (ABC) fields [<a ref-type="bibr" href="#j_nuka-2023-0004_ref_004">4</a>, <a ref-type="bibr" href="#j_nuka-2023-0004_ref_005">5</a>] have recently been proposed as an alternative candidate [<a ref-type="bibr" href="#j_nuka-2023-0004_ref_006">6</a>–<a ref-type="bibr" href="#j_nuka-2023-0004_ref_008">8</a>].
Owing to the improvements in computational power, we can study the properties of magnetic reconnection by practicing numerical simulation. Based on the ABC fields, we particularly focus on the difference in the behaviors of electrons and ions, especially their kinetic energy gains.
</sec>
<sec id="j_nuka-2023-0004_s_002">
<div>Simulation setup</div>
We performed particle-in-cell (PIC) numerical simulations using the Zeltron code<a ref-type="fn" href="#j_nuka-2023-0004_fn_001">(1)</a> [<a ref-type="bibr" href="#j_nuka-2023-0004_ref_009">9</a>] of 2-D periodic magnetic equilibria known as the ABC fields [<a ref-type="bibr" href="#j_nuka-2023-0004_ref_010">10</a>–<a ref-type="bibr" href="#j_nuka-2023-0004_ref_012">12</a>]:
<disp-formula id="j_nuka-2023-0004_eq_001">
<label>1</label>
<alternatives>
<graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="graphic/j_nuka-2023-0004_eq_001.png"></graphic>
<math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="block"><mrow><mtable columnalign="right left right left right left right left right left right left" rowspacing="3pt" columnspacing="0em 2em 0em 2em 0em 2em 0em 2em 0em 2em 0em" displaystyle="true"><mtr><mtd></mtd><mtd><msub><mrow><mi>B</mi></mrow><mrow><mi>x</mi></mrow></msub><mo>=</mo><msub><mrow><mi>B</mi></mrow><mrow><mn>1</mn></mrow></msub><mrow><mo>[</mo><mi>sin</mi><mo>⁡</mo><mrow><mo>(</mo><msub><mrow><mi>α</mi></mrow><mrow><mn>0</mn></mrow></msub><mo stretchy="false">(</mo><mi>x</mi><mo>+</mo><mi>y</mi><mo stretchy="false">)</mo><mo>)</mo></mrow><mo>+</mo><mi>sin</mi><mo>⁡</mo><mrow><mo>(</mo><msub><mrow><mi>α</mi></mrow><mrow><mn>0</mn></mrow></msub><mo stretchy="false">(</mo><mi>x</mi><mo>−</mo><mi>y</mi><mo stretchy="false">)</mo><mo>)</mo></mrow><mo>]</mo></mrow><mo>/</mo><msqrt><mn>2</mn></msqrt></mtd></mtr><mtr><mtd></mtd><mtd><msub><mrow><mi>B</mi></mrow><mrow><mi>y</mi></mrow></msub><mo>=</mo><msub><mrow><mi>B</mi></mrow><mrow><mn>0</mn></mrow></msub><mrow><mo>[</mo><mi>sin</mi><mo>⁡</mo><mrow><mo>(</mo><msub><mrow><mi>α</mi></mrow><mrow><mn>0</mn></mrow></msub><mo stretchy="false">(</mo><mi>x</mi><mo>−</mo><mi>y</mi><mo stretchy="false">)</mo><mo>)</mo></mrow><mo>−</mo><mi>sin</mi><mo>⁡</mo><mrow><mo>(</mo><msub><mrow><mi>α</mi></mrow><mrow><mn>0</mn></mrow></msub><mo stretchy="false">(</mo><mi>x</mi><mo>+</mo><mi>y</mi><mo stretchy="false">)</mo><mo>)</mo></mrow><mo>]</mo></mrow><mo>/</mo><msqrt><mn>2</mn></msqrt></mtd></mtr><mtr><mtd></mtd><mtd><msub><mrow><mi>B</mi></mrow><mrow><mi>z</mi></mrow></msub><mo>=</mo><msub><mrow><mi>B</mi></mrow><mrow><mn>0</mn></mrow></msub><mrow><mo>[</mo><mi>cos</mi><mo>⁡</mo><mrow><mo>(</mo><msub><mrow><mi>α</mi></mrow><mrow><mn>0</mn></mrow></msub><mo stretchy="false">(</mo><mi>x</mi><mo>+</mo><mi>y</mi><mo stretchy="false">)</mo><mo>)</mo></mrow><mo>−</mo><mi>cos</mi><mo>⁡</mo><mrow><mo>(</mo><msub><mrow><mi>α</mi></mrow><mrow><mn>0</mn></mrow></msub><mo stretchy="false">(</mo><mi>x</mi><mo>−</mo><mi>y</mi><mo stretchy="false">)</mo><mo>)</mo></mrow><mo>]</mo></mrow></mtd></mtr></mtable></mrow></math>
<tex-math>\begin{aligned} &amp; B_x=B_1\left[\sin \left(\alpha_0(x+y)\right)+\sin \left(\alpha_0(x-y)\right)\right] / \sqrt{2} \\ &amp; B_y=B_0\left[\sin \left(\alpha_0(x-y)\right)-\sin \left(\alpha_0(x+y)\right)\right] / \sqrt{2} \\ &amp; B_z=B_0\left[\cos \left(\alpha_0(x+y)\right)-\cos \left(\alpha_0(x-y)\right)\right] \end{aligned}</tex-math>
</alternatives>
</disp-formula>
where <italic>α</italic>0 = 2<italic>πk</italic>eff/<italic>L</italic> for the linear domain size <italic>L</italic> and <inline-formula><alternatives><inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="graphic/j_nuka-2023-0004_ieq_001.png"></inline-graphic><math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><msub><mrow><mi>k</mi></mrow><mrow><mtext>eff </mtext></mrow></msub><mo>=</mo><msqrt><mn>2</mn></msqrt></mrow></math><tex-math>$${k_{{\rm{eff}}}} = \sqrt 2 $$</tex-math></alternatives></inline-formula> is the effective wavenumber.
The particle density is given by the expression
<disp-formula id="j_nuka-2023-0004_eq_002">
<label>2</label>
<alternatives>
<graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="graphic/j_nuka-2023-0004_eq_002.png"></graphic>
<math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="block"><mrow><mi>n</mi><mo>=</mo><mfrac><mrow><mn>3</mn><msqrt><mn>2</mn></msqrt><msub><mrow><mi>α</mi></mrow><mrow><mn>0</mn></mrow></msub><msub><mrow><mi>B</mi></mrow><mrow><mn>0</mn></mrow></msub></mrow><mrow><mn>4</mn><mi>π</mi><mi>e</mi><msub><mrow><mover><mrow><mi>a</mi></mrow><mrow><mo stretchy="false">~</mo></mrow></mover></mrow><mrow><mn>1</mn></mrow></msub><mo fence="false" stretchy="false">⟨</mo><mi>β</mi><mo fence="false" stretchy="false">⟩</mo></mrow></mfrac></mrow></math>
<tex-math>$$n = {{3\sqrt 2 {\alpha _0}{B_0}} \over {4\pi e{{\tilde a}_1}\left\langle \beta \right\rangle }}$$</tex-math>
</alternatives>
</disp-formula>
where 〈β〉 is the average dimensionless speed of ions and electrons, and <inline-formula><alternatives><inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="graphic/j_nuka-2023-0004_ieq_002.png"></inline-graphic><math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><msub><mover accent="true"><mi>a</mi><mo>˜</mo></mover><mn>1</mn></msub><mo>≤</mo><mtext>½</mtext></mrow></math><tex-math>${\mathop a\limits^ \sim _1} \le {\raise0.5ex\hbox{$\scriptstyle 1$}
\kern-0.1em/\kern-0.15em
\lower0.25ex\hbox{$\scriptstyle 2$}}$</tex-math></alternatives></inline-formula> is a constant that normalizes the dipole moment of the local particle distribution. The initial total mean magnetization is given as follows:
<disp-formula id="j_nuka-2023-0004_eq_003">
<label>3</label>
<alternatives>
<graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="graphic/j_nuka-2023-0004_eq_003.png"></graphic>
<math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="block"><mrow><mrow><mo>⟨</mo><msub><mrow><mi>σ</mi></mrow><mrow><mi mathvariant="normal">i</mi><mi mathvariant="normal">n</mi><mi mathvariant="normal">i</mi></mrow></msub><mo>⟩</mo></mrow><mo>=</mo><mfrac><mrow><mn>2</mn><msqrt><mn>2</mn></msqrt><msub><mrow><mover><mrow><mi>a</mi></mrow><mrow><mo stretchy="false">~</mo></mrow></mover></mrow><mrow><mn>1</mn></mrow></msub><mo fence="false" stretchy="false">⟨</mo><mi>β</mi><mo fence="false" stretchy="false">⟩</mo></mrow><mrow><mn>3</mn><mrow><mo>[</mo><msub><mrow><mi>C</mi></mrow><mrow><mi mathvariant="normal">w</mi><mo>,</mo><mi mathvariant="normal">i</mi></mrow></msub><mrow><mo>(</mo><msub><mrow><mi mathvariant="normal">Θ</mi></mrow><mrow><mi>i</mi></mrow></msub><mo>)</mo></mrow><mi>μ</mi><mo>+</mo><msub><mrow><mi>C</mi></mrow><mrow><mi mathvariant="normal">w</mi><mo>,</mo><mi mathvariant="normal">e</mi></mrow></msub><mrow><mo>(</mo><msub><mrow><mi mathvariant="normal">Θ</mi></mrow><mrow><mi mathvariant="normal">e</mi></mrow></msub><mo>)</mo></mrow><mo>]</mo></mrow><msub><mrow><mi>α</mi></mrow><mrow><mn>0</mn></mrow></msub><msub><mrow><mi>ρ</mi></mrow><mrow><mi mathvariant="normal">e</mi></mrow></msub></mrow></mfrac></mrow></math>
<tex-math>$$\left\langle {{\sigma _{{\rm{ini}}}}} \right\rangle = {{2\sqrt 2 {{\tilde a}_1}\left\langle \beta \right\rangle } \over {3\left[ {{C_{{\rm{w}},{\rm{i}}}}({{\rm{\Theta }}_i})\mu + {C_{{\rm{w}},{\rm{e}}}}({{\rm{\Theta }}_{\rm{e}}})} \right]{\alpha _0}{\rho _{\rm{e}}}}}$$</tex-math>
</alternatives>
</disp-formula>
where <italic>C</italic>w(Θ) = 4Θ + <italic>K</italic>1(1<italic>/</italic>Θ)<italic>/K</italic>2(1<italic>/</italic>Θ) is a function of the dimensionless temperature Θ = <italic>kT/mc</italic>2 and <italic>Kn</italic>(<italic>x</italic>) is the modified Bessel function of the second kind with <italic>n</italic> = 0, 1, 2. In this paper, we use the subscript “i” to represent the parameters related to ions and “e” to represent electrons. Further, ρe = <italic>m</italic>e<italic>c</italic>2/<italic>eB</italic>0 is the electron gyroradius.
We investigate a wide range of relativistic ion temperatures as 10−2 ≤ Θi ≤ 102 and electron temperatures as 10−2 ≤ Θe ≤ 103. We set <italic>B</italic>0 = 1. In order to resolve the degeneration of 〈σini〉 with the temperatures Θi and Θe, we probe <inline-formula><alternatives><inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="graphic/j_nuka-2023-0004_ieq_003.png"></inline-graphic><math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><msub><mrow><mover accent="true"><mrow><mi>a</mi></mrow><mrow><mo stretchy="true">˜</mo></mrow></mover></mrow><mrow><mn>1</mn></mrow></msub></mrow></math><tex-math>$${\mathop a\limits^ \sim _1}$$</tex-math></alternatives></inline-formula> as 0.1, 0.25 (default), and 0.4. We use numerical grids of 20002 and 46082 cells. The particle number per cell per species is 64. The domain size is <italic>L</italic> = 1920ρ0, where ρ0 = min[Θe<italic>m</italic>e<italic>c</italic>2/(<italic>eB</italic>0), μΘi<italic>m</italic>ec2/(<italic>eB</italic>0)] is the nominal gyroradius. Each simulation runs at least 51000 numerical steps.
For kinetic simulations, it is necessary to resolve the gyroradii of both ions and electrons at the same time. Limited by the grid sizes and resolutions of both species of particles, we choose mass ratios of μ = 10,100 instead of the real ion:electron mass ratio 1836. Previous studies configured with mass ratios either as 1836 [<a ref-type="bibr" href="#j_nuka-2023-0004_ref_013">13</a>] or a sequence such as 10, 25, 50, and 1836 [<a ref-type="bibr" href="#j_nuka-2023-0004_ref_014">14</a>]. Differences caused by the choices of the mass ratio can be ignored by simultaneously increasing the electron temperatures, because the plasma magnetization 〈σini〉∝Θe/μ in the limit Θe >> 1.
In conclusion, our configurations yield initial plasma magnetiza tion 〈σini〉 ≲ &lt;14.38.
</sec>
<sec id="j_nuka-2023-0004_s_003">
<div>Results</div>
<sec id="j_nuka-2023-0004_s_003_s_001">
<div>Particle momentum distributions</div>
In <a ref-type="fig" href="#j_nuka-2023-0004_fig_001">Fig. 1</a>, we present the particle momentum distributions <italic>u</italic>2<italic>N</italic>(<italic>u</italic>), where <italic>u</italic> is the dimensionless particle momentum and <italic>N</italic>(<italic>u</italic>) is the particle distribution. The momentum distributions are multiplied with the mass ratio <italic>m</italic>/<italic>m</italic>e, where <italic>m</italic> represents the mass of either the ions or the electrons accordingly. We did up to 50 runs of simulations, but here, we only present three representative simulations based on the value of the initial enthalpy ratio <italic>w</italic>i/<italic>w</italic>e, i.e., whether the enthalpy is ion-dominated, electron-dominated, or equivalently dominated. We find that the question of which particle species dominates in the initial stage is very important, because the peaks of the spectra are directly related to the initial enthalpy ratio. The particle species that dominates the initial enthalpy produces a higher spectral peak.
<figure id="j_nuka-2023-0004_fig_001" position="float" fig-type="figure">
<h2>Fig. 1.</h2>
<figCaption>Particle momentum distributions of three chosen typical simulations, for μ = 100, <inline-formula><alternatives><inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="graphic/j_nuka-2023-0004_ieq_004.png"></inline-graphic><math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><msub><mrow><mover accent="true"><mrow><mi>a</mi></mrow><mrow><mo stretchy="true">˜</mo></mrow></mover></mrow><mrow><mn>1</mn></mrow></msub><mo>=</mo><mn>0.25</mn></mrow></math><tex-math>$${\mathop a\limits^ \sim _1} = 0.25$$</tex-math></alternatives></inline-formula>, and the size = 46082 cells. The initial enthalpy ratio <italic>w</italic>i/<italic>w</italic>e is indicated in each panel with a different color, so as to make it easier to compare with <a ref-type="fig" href="#j_nuka-2023-0004_fig_002">Fig. 2</a>.</figCaption>
<img xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="graphic/j_nuka-2023-0004_fig_001.jpg" src="https://sciendo-parsed.s3.eu-central-1.amazonaws.com/64726138215d2f6c89dc6393/j_nuka-2023-0004_fig_001.jpg?X-Amz-Algorithm=AWS4-HMAC-SHA256&amp;X-Amz-Date=20240725T103321Z&amp;X-Amz-SignedHeaders=host&amp;X-Amz-Expires=18000&amp;X-Amz-Credential=AKIA6AP2G7AKP25APDM2%2F20240725%2Feu-central-1%2Fs3%2Faws4_request&amp;X-Amz-Signature=8d5a3aaee6cfed327bbb585b9be18e87c8e173e4d78f4de0ff5f89fba1e5c118" class="mw-100"/>
</figure>
</sec>
<sec id="j_nuka-2023-0004_s_003_s_002">
<div>Nonthermal fraction evolutions</div>
However, <a ref-type="fig" href="#j_nuka-2023-0004_fig_002">Fig. 2</a> shows that the other species dominates both the nonthermal particle number and the energy fractions, and both species reach a similar level of the maximum particle energy <italic>γ</italic>max (Lorentz factor).
<figure id="j_nuka-2023-0004_fig_002" position="float" fig-type="figure">
<h2>Fig. 2.</h2>
<figCaption>Nonthermal number fraction, nonthermal energy fraction, and maximum particle energy <italic>γ</italic>max for the cases shown in <a ref-type="fig" href="#j_nuka-2023-0004_fig_001">Fig. 1</a>.</figCaption>
<img xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="graphic/j_nuka-2023-0004_fig_002.jpg" src="https://sciendo-parsed.s3.eu-central-1.amazonaws.com/64726138215d2f6c89dc6393/j_nuka-2023-0004_fig_002.jpg?X-Amz-Algorithm=AWS4-HMAC-SHA256&amp;X-Amz-Date=20240725T103321Z&amp;X-Amz-SignedHeaders=host&amp;X-Amz-Expires=18000&amp;X-Amz-Credential=AKIA6AP2G7AKP25APDM2%2F20240725%2Feu-central-1%2Fs3%2Faws4_request&amp;X-Amz-Signature=0f4f864a09e467890352f0179741a27b3d67641ede8a4deddc9745e7b36e777c" class="mw-100"/>
</figure>
</sec>
<sec id="j_nuka-2023-0004_s_003_s_003">
<div>Kinetic energy partitions</div>
In <a ref-type="fig" href="#j_nuka-2023-0004_fig_003">Fig. 3</a>, we show the kinetic energy partition between ions and electrons. We find that a significant part of our results does not agree with those of previous studies [<a ref-type="bibr" href="#j_nuka-2023-0004_ref_013">13</a>, <a ref-type="bibr" href="#j_nuka-2023-0004_ref_014">14</a>]. Our results show that the energy partition is strongly connected with the initial enthalpy ratio <italic>w</italic>i/<italic>w</italic>e instead of the initial ion cold magnetization <inline-formula><alternatives><inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="graphic/j_nuka-2023-0004_ieq_005.png"></inline-graphic><math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><msub><mrow><mi>σ</mi></mrow><mrow><mtext>i</mtext></mrow></msub><mo>=</mo><msubsup><mrow><mi>B</mi></mrow><mrow><mn>0</mn></mrow><mrow><mn>2</mn></mrow></msubsup><mo>/</mo><mn>4</mn><mtext>π</mtext><mi>n</mi><msub><mrow><mi>m</mi></mrow><mrow><mtext>i</mtext></mrow></msub><msup><mrow><mi>c</mi></mrow><mrow><mn>2</mn></mrow></msup></mrow></math><tex-math>$\sigma _{\rm{i}} = B_0^2 /4{\rm{\pi }}nm_{\rm{i}} c^2 $</tex-math></alternatives></inline-formula> or the initial total hot magnetization 〈σini〉, such that the species dominating the initial enthalpy also dominates the kinetic partition.
<figure id="j_nuka-2023-0004_fig_003" position="float" fig-type="figure">
<h2>Fig. 3.</h2>
<figCaption>The left panel shows the dependence of <italic>q</italic>e on the initial enthalpy ratio <italic>w</italic>i/<italic>w</italic>e. The middle and right panels compare the relative gains <italic>q</italic>e of the electron’s kinetic energies with the results of previous studies (dashed lines). The marker styles and colors are indicated in the figure.</figCaption>
<img xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="graphic/j_nuka-2023-0004_fig_003.jpg" src="https://sciendo-parsed.s3.eu-central-1.amazonaws.com/64726138215d2f6c89dc6393/j_nuka-2023-0004_fig_003.jpg?X-Amz-Algorithm=AWS4-HMAC-SHA256&amp;X-Amz-Date=20240725T103321Z&amp;X-Amz-SignedHeaders=host&amp;X-Amz-Expires=18000&amp;X-Amz-Credential=AKIA6AP2G7AKP25APDM2%2F20240725%2Feu-central-1%2Fs3%2Faws4_request&amp;X-Amz-Signature=f1549ed3e4baec2f54be794222fc8dc28fb979aa92368577d744d8659e84233d" class="mw-100"/>
</figure>
</sec>
</sec>
<sec id="j_nuka-2023-0004_s_004">
<div>Conclusion</div>
In this contribution, we show that the initial ion–electron enthalpy ratio determines the partition of kinetic energy between the particle species, such that the species dominating the initial enthalpy also dominates the peak of the spectra and the kinetic energy gains. However, because both species reach a similar level of the maximum particle energy by the end of the simulations, the species not dominating the initial enthalpy dominates the nonthermal particle number fractions and the nonthermal energy fractions. These results differ from the findings of previous studies, because not all our results follow their predicted trends. One most likely reason is that the majority of the previous papers’ choices of the ion–electron temperature combinations are limited in or near the relation Θi = Θe/μ, but the cases other than this relation are not taken into consideration. On the other hand, our results cover relatively larger temperature combinations. Meanwhile, we are currently analyzing whether these differences may also result from using different initial magnetic field configurations.
</sec>
</div>

Kinetic energy partitions in electron–ion PIC simulations of ABC fields

Nukleonika

This work is licensed under the Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License.

{"article-title":"Kinetic energy partitions in electron\u2013ion PIC simulations of ABC fields"}

We explore the kinetic energy partitions between electrons and ions in the 2-D magnetostatic equilibria called Arnold–Beltrami–Childress (ABC) fields, using...

Kinetic energy partitions in electron–ion PIC simulations of ABC fields

Article Category: ORIGINAL PAPER

Published Online: Apr 03, 2023

Page range: 25 - 28

Received: Jul 15, 2022

Accepted: Nov 18, 2022

DOI: https://doi.org/10.2478/nuka-2023-0004

Keywords
Acceleration of particles, Magnetic reconnection, Relativisitc processes, Simulations

© 2023 Qiang Chen, published by Sciendo

This work is licensed under the Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License.

Kinetic energy partitions in electron–ion PIC simulations of ABC fields

Article Category: ORIGINAL PAPER

Published Online: Apr 03, 2023

Page range: 25 - 28

Received: Jul 15, 2022

Accepted: Nov 18, 2022

DOI: https://doi.org/10.2478/nuka-2023-0004

KeywordsAcceleration of particles, Magnetic reconnection, Relativisitc processes, Simulations

© 2023 Qiang Chen, published by Sciendo

This work is licensed under the Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License.

Keywords
Acceleration of particles, Magnetic reconnection, Relativisitc processes, Simulations