Pressure-strain interaction in plasma turbulence: Contribution of the ion non-gyrotropy

Result code in IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F25%3A00643670" target="_blank" >RIV/67985815:_____/25:00643670 - isvavai.cz</a>

Alternative codes found

RIV/68378289:_____/25:00643657

Result on the web

<a href="https://hdl.handle.net/11104/0373572" target="_blank" >https://hdl.handle.net/11104/0373572</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1051/0004-6361/202556752" target="_blank" >10.1051/0004-6361/202556752</a>

Result language

angličtina

Original language name

Pressure-strain interaction in plasma turbulence: Contribution of the ion non-gyrotropy

Original language description

We investigated the properties of plasma turbulence at ion scales in the context of the solar wind. We concentrated on the pressure-strain coupling between the kinetic and magnetic energy and the internal energy, we analysed its capability to produce an effectively irreversible transfer towards the internal energy. Methods. We studied results from a three-dimensional hybrid simulation of decaying turbulence when protons exhibit a substantial temperature anisotropy. We analysed the time evolution and behaviour of the combined (magnetic plus kinetic) energy and its spectral properties. Using the Kármán-Howarth-Monin (KHM) formalism, we quantified the role of the dissipation via the resistive channel and that of the pressure-strain term in generating internal energy. Results. The combined energy flows from large to intermediate and small scales, where it is efficiently dissipated via the resistive term and is exchanged with the internal energy through the pressure-strain term. The pressure-strain coupling oscillates strongly, and this oscillation reflects its reversibility properties that are embedded in a secular evolution towards a global increase in the plasma internal energy. All the terms involved in the KHM energy balance equation are strongly anisotropic with respect to the mean magnetic field. They tend to be elongated along the mean magnetic field and oscillate over time at large scales, which is connected with the pressure-strain coupling. The reversible oscillatory part of the pressure-strain coupling is mostly contained in the gyrotropic pressure-strain part. This mainly affects the turbulent processes at large scales, but when it is time averaged, it also contributes to the ion energisation approximately at ion scales. The non-gyrotropic pressure-strain part does not oscillate significantly, acts at ion scales, and can be considered as the main effective dissipation channel.

Czech name

—

Czech description

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Type

J_imp - Article in a specialist periodical, which is included in the Web of Science database

CEP classification

—

OECD FORD branch

10308 - Astronomy (including astrophysics,space science)

Project

<a href="/en/project/GA25-17802S" target="_blank" >GA25-17802S: Plasma turbulence in the solar wind</a><br>

Continuities

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Publication year

2025

Confidentiality

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Name of the periodical

Astronomy & Astrophysics

ISSN

0004-6361

e-ISSN

1432-0746

Volume of the periodical

704

Issue of the periodical within the volume

Dec.

Country of publishing house

FR - FRANCE

Number of pages

8

Pages from-to

A131

UT code for WoS article

001631789300023

EID of the result in the Scopus database

2-s2.0-105024067223