Magnetopause Location Under Influence of Large Solar Wind Structures

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F19%3A10406370" target="_blank" >RIV/00216208:11320/19:10406370 - isvavai.cz</a>

Výsledek na webu

<a href="https://www.mff.cuni.cz/veda/konference/wds/proc/pdf19/WDS19_22_f2_Salohub.pdf" target="_blank" >https://www.mff.cuni.cz/veda/konference/wds/proc/pdf19/WDS19_22_f2_Salohub.pdf</a>

DOI - Digital Object Identifier

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Jazyk výsledku

angličtina

Název v původním jazyce

Magnetopause Location Under Influence of Large Solar Wind Structures

Popis výsledku v původním jazyce

We investigate the magnetopause (MP) location influenced by large solar wind (SW) structures: magnetic clouds (MCs), interplanetary coronal mass ejections (ICMEs), and intervals following interplanetary shocks (IPs) driven by these structures and compare it with the MP location in the pristine SW. We focus on the differences between predicted and encountered MP locations near the subsolar point. For predictions, we used the MP model of Shue et al. [1997] where Wind plasma and magnetic field parameters from 2007 to 2015 have been applied as input data. Into the model, we added other pressure components reflecting the different alpha particle content and larger magnetic field. We found that differences between the modeled and observed (by the THEMIS spacecraft) MP locations in the subsolar region are small but systematic. We discuss changes in model predictions and other factors which are not included in the model but can affect of the magnetopause location (for example, geomagnetic activity demonstrated by SYM-H and AE indices in our case).

Název v anglickém jazyce

Magnetopause Location Under Influence of Large Solar Wind Structures

Popis výsledku anglicky

We investigate the magnetopause (MP) location influenced by large solar wind (SW) structures: magnetic clouds (MCs), interplanetary coronal mass ejections (ICMEs), and intervals following interplanetary shocks (IPs) driven by these structures and compare it with the MP location in the pristine SW. We focus on the differences between predicted and encountered MP locations near the subsolar point. For predictions, we used the MP model of Shue et al. [1997] where Wind plasma and magnetic field parameters from 2007 to 2015 have been applied as input data. Into the model, we added other pressure components reflecting the different alpha particle content and larger magnetic field. We found that differences between the modeled and observed (by the THEMIS spacecraft) MP locations in the subsolar region are small but systematic. We discuss changes in model predictions and other factors which are not included in the model but can affect of the magnetopause location (for example, geomagnetic activity demonstrated by SYM-H and AE indices in our case).

Druh

D - Stať ve sborníku

CEP obor

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OECD FORD obor

10305 - Fluids and plasma physics (including surface physics)

Projekt

<a href="/cs/project/GA17-06065S" target="_blank" >GA17-06065S: Variace slunečního větru a jejich vazba na dynamiku magnetosféry Země</a><br>

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 statě ve sborníku

WDS&apos;19 Proceedings of Contributed Papers — Physics

ISBN

978-80-7378-409-6

ISSN

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e-ISSN

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Počet stran výsledku

7

Strana od-do

124-130

Název nakladatele

Matfyzpress

Místo vydání

Praha

Místo konání akce

Praha

Datum konání akce

4. 6. 2019

Typ akce podle státní příslušnosti

EUR - Evropská akce

Kód UT WoS článku

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