Turbulent Energy Dissipation at Fast Interplanetary Shocks: Solar Orbiter and Wind Observations

Result code in IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F24%3A10493202" target="_blank" >RIV/00216208:11320/24:10493202 - isvavai.cz</a>

Result on the web

<a href="https://physics.mff.cuni.cz/wds/proc/pdf24/WDS24_10_f2_Park.pdf" target="_blank" >https://physics.mff.cuni.cz/wds/proc/pdf24/WDS24_10_f2_Park.pdf</a>

DOI - Digital Object Identifier

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Result language

angličtina

Original language name

Turbulent Energy Dissipation at Fast Interplanetary Shocks: Solar Orbiter and Wind Observations

Original language description

We present an analysis of turbulence evolution at interplanetary (IP) shocksobserved by Solar Orbiter (at ALMOST EQUAL TO 0.5 au) and Wind (at 1 au). IP shocks formed byinterplanetary coronal mass ejections (ICMEs) and stream interaction regions (SIRs)are critical sites for wave generation and particle acceleration in the heliosphere.The energy dissipation of solar wind turbulence in small scales is affected by variousquantities, such as cross-helicity. Using two fast forward (FF) and reverse (FR)shock pairs, we examine the evolution of turbulence, focusing on the transition rangespectral index (αtr) and its dependence on shock-related processes. We reveal abruptchanges in plasma properties across shocks, supporting the hypothesis that IP shocksact as thin boundaries between distinct plasma regions. In the upstream of a nearlyoblique FF shock at Solar Orbiter compared to other quasi-perpendicular shocks,spectral steepening is likely driven by wave activities associated with backstreamingparticles reflected from the shock. Furthermore, αtr generally shows little correlationwith local plasma parameters. This suggests that wave-particle interaction ratherthan local plasma variations govern turbulent energy dissipation at shocks, and waveactivities need to be considered in defining the &apos;effective thickness&apos; of collisionlessshocks. Our results extend insights into the broader role of shocks in modulatingenergy transfer in the heliosphere.

Czech name

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Czech description

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Type

D - Article in proceedings

CEP classification

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OECD FORD branch

10305 - Fluids and plasma physics (including surface physics)

Project

<a href="/en/project/GA23-06401S" target="_blank" >GA23-06401S: Where and how the solar wind is accelerated and heated and how these processes affect its evolution?</a><br>

Continuities

P - Projekt vyzkumu a vyvoje financovany z verejnych zdroju (s odkazem do CEP)

Publication year

2024

Confidentiality

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

Article name in the collection

WDS&apos;24 Proceedings of Contributed Papers - Physics

ISBN

978-80-7378-520-8

ISSN

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e-ISSN

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Number of pages

10

Pages from-to

72-81

Publisher name

Matfyzpress

Place of publication

Praha

Event location

Praha

Event date

Jun 4, 2024

Type of event by nationality

EUR - Evropská akce

UT code for WoS article

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