dorsal/arxiv
View SchemaCascade Processes of Strong and Weak MHD Turbulence
| Authors | Na-Na Gao, Jian-Fu Zhang, Jungyeon Cho |
|---|---|
| Categories | |
| ArXiv ID | 2601.08093vv1 |
| URL | https://arxiv.org/abs/2601.08093 |
| License | http://creativecommons.org/licenses/by/4.0/ |
Abstract
On the framework of relativistic force-free magnetohydrodynamic (MHD) turbulence, we explore the fundamental properties of strong and weak turbulent cascades using high-resolution numerical simulations in the presence of a uniform background magnetic field. We find that (1) power spectra and scale-dependent anisotropies both for the strong and weak turbulence resemble those observed in the non-relativistic MHD turbulence; (2) intermittency of magnetic fields in strong turbulence is stronger than that in the weak one; (3) generated Alfv\'en modes show similar energy spectra and scale-dependent anisotropies to those of non-relativistic case; (4) generated fast modes present a power spectrum similar to that of Alfv\'en modes, with a strong (for strong turbulence) or weak (for weak turbulence) scale-dependent anisotropy, which are significantly different from non-relativistic turbulence; and (5) applications of our numerical results to neutron star magnetospheres show that the strong (or moderately weak) turbulent cascade can explain the X-ray radiation of the Vela pulsar. Our study is of great significance for understanding energy transfer, magnetic field evolution, and particle acceleration mechanisms in extreme astrophysical environments.
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"abstract": "On the framework of relativistic force-free magnetohydrodynamic (MHD) turbulence, we explore the fundamental properties of strong and weak turbulent cascades using high-resolution numerical simulations in the presence of a uniform background magnetic field. We find that (1) power spectra and scale-dependent anisotropies both for the strong and weak turbulence resemble those observed in the non-relativistic MHD turbulence; (2) intermittency of magnetic fields in strong turbulence is stronger than that in the weak one; (3) generated Alfv\\\u0027en modes show similar energy spectra and scale-dependent anisotropies to those of non-relativistic case; (4) generated fast modes present a power spectrum similar to that of Alfv\\\u0027en modes, with a strong (for strong turbulence) or weak (for weak turbulence) scale-dependent anisotropy, which are significantly different from non-relativistic turbulence; and (5) applications of our numerical results to neutron star magnetospheres show that the strong (or moderately weak) turbulent cascade can explain the X-ray radiation of the Vela pulsar. Our study is of great significance for understanding energy transfer, magnetic field evolution, and particle acceleration mechanisms in extreme astrophysical environments.",
"arxiv_id": "2601.08093",
"authors": [
"Na-Na Gao",
"Jian-Fu Zhang",
"Jungyeon Cho"
],
"categories": [
"astro-ph.HE"
],
"license": "http://creativecommons.org/licenses/by/4.0/",
"title": "Cascade Processes of Strong and Weak MHD Turbulence",
"url": "https://arxiv.org/abs/2601.08093",
"version": "v1"
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