Fine Structure of Interplanetary Shock Front-Results from BMSW Experiment with High Time Resolution

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F19%3A10405938" target="_blank" >RIV/00216208:11320/19:10405938 - isvavai.cz</a>

Výsledek na webu

<a href="https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=8Gv5R~X7n" target="_blank" >https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=8Gv5R~X7n</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1029/2018JA026255" target="_blank" >10.1029/2018JA026255</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Fine Structure of Interplanetary Shock Front-Results from BMSW Experiment with High Time Resolution

Popis výsledku v původním jazyce

The structure of subcritical interplanetary shocks was studied using high time resolution from the BMSW plasma instrument onboard the Spektr-R satellite and MFI magnetometer measurements from WIND. Ion scales of the ramp and wavelength of precursor waves were obtained and compared with results of the bow shock structure study. The comparison of precursor wavelengths, determined experimentally with those determined from dispersion relation for low-Mach, low-beta shocks has showed similar results. This confirms the assumption that the dispersion of oblique magnetosonic waves is the determining factor in the formation of upstream wave trains. On the base of the case study it was shown that damped downstream oscillations of density, velocity, temperature may be generated by the interaction of the inflowing solar wind ions with the reflected gyrating ions inside the ramp. A sequence of six wave trains of magnetosonic whistlers has been observed upstream the ramp of subcritical oblique IP shock. The amplitude of oscillations inside the trains decreased with increasing distance from the ramp. The possible energy dissipation mechanism within the shock front is discussed.

Název v anglickém jazyce

Fine Structure of Interplanetary Shock Front-Results from BMSW Experiment with High Time Resolution

Popis výsledku anglicky

The structure of subcritical interplanetary shocks was studied using high time resolution from the BMSW plasma instrument onboard the Spektr-R satellite and MFI magnetometer measurements from WIND. Ion scales of the ramp and wavelength of precursor waves were obtained and compared with results of the bow shock structure study. The comparison of precursor wavelengths, determined experimentally with those determined from dispersion relation for low-Mach, low-beta shocks has showed similar results. This confirms the assumption that the dispersion of oblique magnetosonic waves is the determining factor in the formation of upstream wave trains. On the base of the case study it was shown that damped downstream oscillations of density, velocity, temperature may be generated by the interaction of the inflowing solar wind ions with the reflected gyrating ions inside the ramp. A sequence of six wave trains of magnetosonic whistlers has been observed upstream the ramp of subcritical oblique IP shock. The amplitude of oscillations inside the trains decreased with increasing distance from the ramp. The possible energy dissipation mechanism within the shock front is discussed.

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

2019

Kód důvěrnosti údajů

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

Název periodika

Journal of Geophysical Research: Space Physics

ISSN

2169-9380

e-ISSN

—

Svazek periodika

124

Číslo periodika v rámci svazku

11

Stát vydavatele periodika

US - Spojené státy americké

Počet stran výsledku

17

Strana od-do

—

Kód UT WoS článku

000494533100001

EID výsledku v databázi Scopus

2-s2.0-85074856632