Density Fluctuations in the Solar Wind Driven by Alfven Wave Parametric Decay

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F18%3A00496116" target="_blank" >RIV/67985815:_____/18:00496116 - isvavai.cz</a>

Výsledek na webu

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

DOI - Digital Object Identifier

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

Jazyk výsledku

angličtina

Název v původním jazyce

Density Fluctuations in the Solar Wind Driven by Alfven Wave Parametric Decay

Popis výsledku v původním jazyce

Measurements and simulations of inertial compressive turbulence in the solar wind are characterized by anti-correlated magnetic fluctuations parallel to the mean field and density structures. This signature has been interpreted as observational evidence for non-propagating pressure balanced structures, kinetic ion-acoustic waves, as well as the MHD slow-mode. Given the high damping rates of parallel propagating compressive fluctuations, their ubiquity in satellite observations is surprising and suggestive of a local driving process. One possible candidate for the generation of compressive fluctuations in the solar wind is the Alfven wave parametric instability. Here, we test the parametric decay process as a source of compressive waves in the solar wind by comparing the collisionless damping rates of compressive fluctuations with growth rates of the parametric decay instability daughter waves. Our results suggest that generation of compressive waves through parametric decay is overdamped at 1 au, but that the presence of slow-mode-like density fluctuations is correlated with the parametric decay of Alfven waves.

Název v anglickém jazyce

Density Fluctuations in the Solar Wind Driven by Alfven Wave Parametric Decay

Popis výsledku anglicky

Measurements and simulations of inertial compressive turbulence in the solar wind are characterized by anti-correlated magnetic fluctuations parallel to the mean field and density structures. This signature has been interpreted as observational evidence for non-propagating pressure balanced structures, kinetic ion-acoustic waves, as well as the MHD slow-mode. Given the high damping rates of parallel propagating compressive fluctuations, their ubiquity in satellite observations is surprising and suggestive of a local driving process. One possible candidate for the generation of compressive fluctuations in the solar wind is the Alfven wave parametric instability. Here, we test the parametric decay process as a source of compressive waves in the solar wind by comparing the collisionless damping rates of compressive fluctuations with growth rates of the parametric decay instability daughter waves. Our results suggest that generation of compressive waves through parametric decay is overdamped at 1 au, but that the presence of slow-mode-like density fluctuations is correlated with the parametric decay of Alfven waves.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

<a href="/cs/project/GA18-08861S" target="_blank" >GA18-08861S: Plazmová turbulence na iontových škálách ve slunečním větru</a><br>

Návaznosti

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

Rok uplatnění

2018

Kód důvěrnosti údajů

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

Název periodika

Astrophysical Journal Letters

ISSN

2041-8213

e-ISSN

—

Svazek periodika

854

Číslo periodika v rámci svazku

2

Stát vydavatele periodika

GB - Spojené království Velké Británie a Severního Irska

Počet stran výsledku

6

Strana od-do

—

Kód UT WoS článku

000426055900006

EID výsledku v databázi Scopus

2-s2.0-85047737260