Modification of the Power Spectral Density of Magnetic Field Fluctuations by Quasi-perpendicular Interplanetary Shocks

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F25%3A10501547" target="_blank" >RIV/00216208:11320/25:10501547 - isvavai.cz</a>

Výsledek na webu

<a href="https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=Y_SIz3RjIT" target="_blank" >https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=Y_SIz3RjIT</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.3847/2041-8213/ade25b" target="_blank" >10.3847/2041-8213/ade25b</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Modification of the Power Spectral Density of Magnetic Field Fluctuations by Quasi-perpendicular Interplanetary Shocks

Popis výsledku v původním jazyce

We investigate the role of interplanetary (IP) shocks in solar wind turbulence using observations of Solar Orbiter, Parker Solar Probe, and Wind. Employing statistical analysis of quasi-perpendicular fast forward (FF) and fast reverse (FR) shocks, we revisit evolution of magnetic field turbulence across IP shocks. Our previous work indicates that the spectral properties of magnetic fluctuations are statistically conserved across different types of IP shocks, except FR shocks in the transition range of frequencies. We focus on the spectral index in the transition range ( alpha tr ) using 1 minute sliding windows at 10 s intervals to probe the turbulent dissipation near shocks. We address the influence of key turbulence parameters, particularly cross helicity (sigma c) and fluctuation amplitude (sigma B), on alpha tr . Our results demonstrate (1) an immediate change in alpha tr across the shock with no evidence for further gradual or asymptotic evolution over extended intervals, and this implies that shock universally serves as a thin boundary separating two turbulence states; (2) the dominant factor forming the steepness of alpha tr is sigma c, rather than sigma B; and (3) the statistically shallower downstream alpha tr of FR shocks results from a systematic reduction in sigma c across shocks. These findings suggest that the observed spectral modification is primarily governed by changes in turbulence Alfv &amp; eacute;nicity, not directly by dissipation processes related to the shock, and can be commonly observed toward extensive heliospheric distances.

Název v anglickém jazyce

Modification of the Power Spectral Density of Magnetic Field Fluctuations by Quasi-perpendicular Interplanetary Shocks

Popis výsledku anglicky

We investigate the role of interplanetary (IP) shocks in solar wind turbulence using observations of Solar Orbiter, Parker Solar Probe, and Wind. Employing statistical analysis of quasi-perpendicular fast forward (FF) and fast reverse (FR) shocks, we revisit evolution of magnetic field turbulence across IP shocks. Our previous work indicates that the spectral properties of magnetic fluctuations are statistically conserved across different types of IP shocks, except FR shocks in the transition range of frequencies. We focus on the spectral index in the transition range ( alpha tr ) using 1 minute sliding windows at 10 s intervals to probe the turbulent dissipation near shocks. We address the influence of key turbulence parameters, particularly cross helicity (sigma c) and fluctuation amplitude (sigma B), on alpha tr . Our results demonstrate (1) an immediate change in alpha tr across the shock with no evidence for further gradual or asymptotic evolution over extended intervals, and this implies that shock universally serves as a thin boundary separating two turbulence states; (2) the dominant factor forming the steepness of alpha tr is sigma c, rather than sigma B; and (3) the statistically shallower downstream alpha tr of FR shocks results from a systematic reduction in sigma c across shocks. These findings suggest that the observed spectral modification is primarily governed by changes in turbulence Alfv &amp; eacute;nicity, not directly by dissipation processes related to the shock, and can be commonly observed toward extensive heliospheric distances.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

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 Letters

ISSN

2041-8205

e-ISSN

2041-8213

Svazek periodika

986

Číslo periodika v rámci svazku

2

Stát vydavatele periodika

US - Spojené státy americké

Počet stran výsledku

7

Strana od-do

L30

Kód UT WoS článku

001512348400001

EID výsledku v databázi Scopus

2-s2.0-105008985370