Ion-scale Turbulence and Energy Cascade Rate in the Solar Corona and Inner Heliosphere

Result code in IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F25%3A10510600" target="_blank" >RIV/00216208:11320/25:10510600 - isvavai.cz</a>

Result on the web

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

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.3847/2041-8213/ae09b0" target="_blank" >10.3847/2041-8213/ae09b0</a>

Result language

angličtina

Original language name

Ion-scale Turbulence and Energy Cascade Rate in the Solar Corona and Inner Heliosphere

Original language description

Plasma turbulence cascading from MHD to kinetic scales in the heliospheric plasma is believed to play a key role in coronal heating and fast solar wind acceleration, but the properties of the turbulence remain poorly constrained by observations. Here we compare the ion-scale density fluctuation levels inferred from the properties of solar radio bursts with the magnetic field fluctuation levels obtained through in situ measurements in the inner heliosphere. We find that the observed magnetic and density fluctuation amplitudes are consistent with excitation by kinetic Alfv &amp; eacute;n waves (KAWs) and/or KAW structures over a broad range of distances from the Sun. We then use the radio diagnostics and the KAW scenario to deduce the radial variation of magnetic fluctuation amplitudes in regions close to the Sun where in situ measurements cannot be obtained. Further, we calculate the energy cascade rate (plasma heating rate) profile over a region that extends from the low corona (similar to 0.1 R circle dot) into the heliosphere (out to similar to 1 au), and compare it to the energy deposition rate required to drive the solar wind. The cascade rate agrees with the available in situ measurements and also provides predictions closer than similar to 10 R circle dot where in situ approaches are not available. The results provide unique diagnostics of the ion-scale plasma turbulence amplitude and energy cascade rate spanning over 3 orders of magnitude in solar distance.

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

10305 - Fluids and plasma physics (including surface physics)

Project

<a href="/en/project/LUAUS25060" target="_blank" >LUAUS25060: How and where is the solar wind accelerated and heated and how do these processes influence its propagation through the heliosphere?</a><br>

Continuities

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

Astrophysical Journal Letters

ISSN

2041-8205

e-ISSN

2041-8213

Volume of the periodical

991

Issue of the periodical within the volume

2

Country of publishing house

US - UNITED STATES

Number of pages

8

Pages from-to

L57

UT code for WoS article

001585176700001

EID of the result in the Scopus database

2-s2.0-105017599025