Investigation of Turbulent Fluctuations in the Fast and Alfvenic Slow Solar Wind at 1 au

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F25%3A10510638" target="_blank" >RIV/00216208:11320/25:10510638 - isvavai.cz</a>

Výsledek na webu

<a href="https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=ITmVYZ2T6x" target="_blank" >https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=ITmVYZ2T6x</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.3847/1538-4357/ae1a85" target="_blank" >10.3847/1538-4357/ae1a85</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Investigation of Turbulent Fluctuations in the Fast and Alfvenic Slow Solar Wind at 1 au

Popis výsledku v původním jazyce

We study the turbulent modes present in the Alfvenic slow and fast solar wind. This analysis focuses on two solar wind intervals: 2022 January 26-29 and February 6-9, and it is based on wind observations at 1 au. Our study examined Alfvenic slow with beta &lt; 1 and fast solar wind with beta &lt; 1 (similar to O(1)), employing a superposed epoch analysis (SEA) to investigate the different turbulent modes and their power spectral densities. We find that the density fluctuations in Alfvenic slow and fast solar wind are primarily fast magnetosonic (MS) modes, although they differ in the dominant propagation direction of fast MS modes-forward propagating in the Alfvenic slow and backward propagating in the fast solar wind. In the Alfvenic slow regime, the SEA shows that the incompressible velocity fluctuations dominate the compressible contributions from fast and slow MS modes. The relative power of velocity fluctuations is largest in backward Alfv &amp; eacute;n propagating modes, similar to 28.8% of the total velocity fluctuations energy. The wavenumber anisotropy of the fast MS modes associated with density fluctuations is k(perpendicular to) &gt;&gt; k(parallel to). In the fast solar wind, compressible velocity fluctuations are dominated by fast MS mode, with the velocity fluctuation energy of 43.6% in backward and 42.0% in forward components, surpassing the contributions from the incompressible Alfvenic fluctuations. We find that magnetic field fluctuations are predominantly associated with magnetic island modes, contributing 53.9% of the total magnetic fluctuations energy in the Alfvenic slow and 35.4% in the fast solar wind.

Název v anglickém jazyce

Investigation of Turbulent Fluctuations in the Fast and Alfvenic Slow Solar Wind at 1 au

Popis výsledku anglicky

We study the turbulent modes present in the Alfvenic slow and fast solar wind. This analysis focuses on two solar wind intervals: 2022 January 26-29 and February 6-9, and it is based on wind observations at 1 au. Our study examined Alfvenic slow with beta &lt; 1 and fast solar wind with beta &lt; 1 (similar to O(1)), employing a superposed epoch analysis (SEA) to investigate the different turbulent modes and their power spectral densities. We find that the density fluctuations in Alfvenic slow and fast solar wind are primarily fast magnetosonic (MS) modes, although they differ in the dominant propagation direction of fast MS modes-forward propagating in the Alfvenic slow and backward propagating in the fast solar wind. In the Alfvenic slow regime, the SEA shows that the incompressible velocity fluctuations dominate the compressible contributions from fast and slow MS modes. The relative power of velocity fluctuations is largest in backward Alfv &amp; eacute;n propagating modes, similar to 28.8% of the total velocity fluctuations energy. The wavenumber anisotropy of the fast MS modes associated with density fluctuations is k(perpendicular to) &gt;&gt; k(parallel to). In the fast solar wind, compressible velocity fluctuations are dominated by fast MS mode, with the velocity fluctuation energy of 43.6% in backward and 42.0% in forward components, surpassing the contributions from the incompressible Alfvenic fluctuations. We find that magnetic field fluctuations are predominantly associated with magnetic island modes, contributing 53.9% of the total magnetic fluctuations energy in the Alfvenic slow and 35.4% in the fast solar wind.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

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OECD FORD obor

10305 - Fluids and plasma physics (including surface physics)

Projekt

Výsledek vznikl pri realizaci vícero projektů. Více informací v záložce Projekty.

Návaznosti

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

Rok uplatnění

2025

Kód důvěrnosti údajů

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

Název periodika

Astrophysical Journal

ISSN

0004-637X

e-ISSN

1538-4357

Svazek periodika

995

Číslo periodika v rámci svazku

2

Stát vydavatele periodika

US - Spojené státy americké

Počet stran výsledku

22

Strana od-do

212

Kód UT WoS článku

001643350800001

EID výsledku v databázi Scopus

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