Evolution of the magnetic field structure outside the magnetopause under radial IMF conditions

Result code in IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F17%3A10371408" target="_blank" >RIV/00216208:11320/17:10371408 - isvavai.cz</a>

Result on the web

<a href="http://dx.doi.org/10.1002/2015JA021809" target="_blank" >http://dx.doi.org/10.1002/2015JA021809</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1002/2015JA021809" target="_blank" >10.1002/2015JA021809</a>

Result language

angličtina

Original language name

Evolution of the magnetic field structure outside the magnetopause under radial IMF conditions

Original language description

We use the Time History of Events and Macroscale Interactions during Substorms data to investigate the magnetic field structure just outside the magnetopause and its time evolution for radial interplanetary magnetic field (IMF) events. When the magnetic field drapes around the magnetopause in the magnetosheath region, an asymmetric magnetic field orientation in different hemispheres is expected. Our two-case study reveals some conflicts with the predicted draped field configuration in the Southern Hemisphere. The magnetosheath B-z component had a different sign depending on the upstream IMF B-x component&apos;s polarity at the beginning of the radial IMF intervals. With time, the observed B-z became northward in both cases with increasing positive values through the events. The increasing value of the B-z component may be explained by two possible mechanisms: by a change of the upstream IMF and by a reconnection between magnetosheath and magnetospheric field lines. Our study shows that both mechanisms contributed to the observed changes. Thus, there was a correlation between the change of the upstream IMF conditions and an increase in the magnetosheath northward magnetic field component. The observed formation of the boundary layer near the magnetopause proves that the reconnection process was ongoing at least for a part of the time. We suggest two possible reconnection scenarios: one near subsolar point and another tailward of the one cusp due to lobe reconnection. The asymmetry of reconnection locations causes rearrangement of the magnetic field structure near the magnetopause and turns the observed magnetosheath B-z component even further into positive values.

Czech name

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Czech description

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Type

J_imp - Article in a specialist periodical, which is included in the Web of Science database

CEP classification

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OECD FORD branch

10305 - Fluids and plasma physics (including surface physics)

Project

<a href="/en/project/GA17-06065S" target="_blank" >GA17-06065S: Solar wind variations and their impact on magnetospheric dynamics</a><br>

Continuities

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

Publication year

2017

Confidentiality

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

Name of the periodical

Journal of Geophysical Research: Space Physics

ISSN

2169-9380

e-ISSN

—

Volume of the periodical

122

Issue of the periodical within the volume

4

Country of publishing house

US - UNITED STATES

Number of pages

13

Pages from-to

4051-4063

UT code for WoS article

000401340800014

EID of the result in the Scopus database

2-s2.0-85017336079