Fine structure of the interplanetary shock front according to measurements of the ion flux of the solar wind with high time resolution

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F17%3A10371307" target="_blank" >RIV/00216208:11320/17:10371307 - isvavai.cz</a>

Výsledek na webu

<a href="http://dx.doi.org/10.1134/S0010952517010038" target="_blank" >http://dx.doi.org/10.1134/S0010952517010038</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1134/S0010952517010038" target="_blank" >10.1134/S0010952517010038</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Fine structure of the interplanetary shock front according to measurements of the ion flux of the solar wind with high time resolution

Popis výsledku v původním jazyce

According to the data of the BMSW/SPEKTR-R instrument, which measured the density and velocity of solar wind plasma with a record time resolution, up to similar to 3 x10(-2) s, the structure of the front of interplanetary shocks has been investigated. The results of these first investigations were compared with the results of studying the structure of the bow shocks obtained in previous years. A comparison has shown that the quasi-stationary (averaged over the rapid oscillations) distribution of plasma behind the interplanetary shock front was significantly more inhomogeneous than that behind the bow-shock front, i.e., in the magnetosheath. It has also been shown that, to determine the size of internal structures of the fronts of quasi-perpendicular (theta(BN) &gt; 45A degrees) shocks, one could use the magnetic field magnitude, the proton density, and the proton flux of the solar wind on almost equal terms. A comparison of low Mach (De (D) &lt; 2), low beta (beta(1) &lt; 1) fronts of interplanetary and bow shocks has shown that the dispersion of oblique magnetosonic waves plays an essential role in their formation.

Název v anglickém jazyce

Fine structure of the interplanetary shock front according to measurements of the ion flux of the solar wind with high time resolution

Popis výsledku anglicky

According to the data of the BMSW/SPEKTR-R instrument, which measured the density and velocity of solar wind plasma with a record time resolution, up to similar to 3 x10(-2) s, the structure of the front of interplanetary shocks has been investigated. The results of these first investigations were compared with the results of studying the structure of the bow shocks obtained in previous years. A comparison has shown that the quasi-stationary (averaged over the rapid oscillations) distribution of plasma behind the interplanetary shock front was significantly more inhomogeneous than that behind the bow-shock front, i.e., in the magnetosheath. It has also been shown that, to determine the size of internal structures of the fronts of quasi-perpendicular (theta(BN) &gt; 45A degrees) shocks, one could use the magnetic field magnitude, the proton density, and the proton flux of the solar wind on almost equal terms. A comparison of low Mach (De (D) &lt; 2), low beta (beta(1) &lt; 1) fronts of interplanetary and bow shocks has shown that the dispersion of oblique magnetosonic waves plays an essential role in their formation.

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

<a href="/cs/project/GA16-04956S" target="_blank" >GA16-04956S: Sluneční vítr jako přírodní laboratoř: struktura, turbulence a rázové vlny.</a><br>

Návaznosti

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

Rok uplatnění

2017

Kód důvěrnosti údajů

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

Název periodika

Cosmic Research (English translation of Kosimicheskie Issledovaniya)

ISSN

0010-9525

e-ISSN

—

Svazek periodika

55

Číslo periodika v rámci svazku

1

Stát vydavatele periodika

RU - Ruská federace

Počet stran výsledku

16

Strana od-do

30-45

Kód UT WoS článku

000394182700004

EID výsledku v databázi Scopus

2-s2.0-85011932298