Investigation of Turbulent Fluctuations in the Fast and Alfvenic Slow Solar Wind at 1 au
The result's identifiers
Result code in 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>
Result on the web
<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>
Alternative languages
Result language
angličtina
Original language name
Investigation of Turbulent Fluctuations in the Fast and Alfvenic Slow Solar Wind at 1 au
Original language description
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 < 1 and fast solar wind with beta < 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 & 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) >> 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.
Czech name
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Czech description
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Classification
Type
J<sub>imp</sub> - Article in a specialist periodical, which is included in the Web of Science database
CEP classification
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OECD FORD branch
10305 - Fluids and plasma physics (including surface physics)
Result continuities
Project
Result was created during the realization of more than one project. More information in the Projects tab.
Continuities
P - Projekt vyzkumu a vyvoje financovany z verejnych zdroju (s odkazem do CEP)
Others
Publication year
2025
Confidentiality
S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů
Data specific for result type
Name of the periodical
Astrophysical Journal
ISSN
0004-637X
e-ISSN
1538-4357
Volume of the periodical
995
Issue of the periodical within the volume
2
Country of publishing house
US - UNITED STATES
Number of pages
22
Pages from-to
212
UT code for WoS article
001643350800001
EID of the result in the Scopus database
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