Over-expansion of coronal mass ejections modelled using 3D MHD EUHFORIA simulations
The result's identifiers
Result code in IS VaVaI
<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F68378289%3A_____%2F22%3A00560526" target="_blank" >RIV/68378289:_____/22:00560526 - isvavai.cz</a>
Result on the web
<a href="https://hal-obspm.ccsd.cnrs.fr/obspm-03905452/document" target="_blank" >https://hal-obspm.ccsd.cnrs.fr/obspm-03905452/document</a>
DOI - Digital Object Identifier
<a href="http://dx.doi.org/10.1016/j.asr.2022.06.013" target="_blank" >10.1016/j.asr.2022.06.013</a>
Alternative languages
Result language
angličtina
Original language name
Over-expansion of coronal mass ejections modelled using 3D MHD EUHFORIA simulations
Original language description
Context: Coronal mass ejections (CMEs) are large-scale eruptions observed close to the Sun. They travel through the heliosphere and possibly interact with the Earth environment, creating interruptions or even damaging new-technology instruments. Most of the time their physical conditions (velocity, density and pressure) are measured in situ at only one point in space, with no possibility of having information on the variation of these parameters during their journey from the Sun to Earth.nAim: Our aim is to understand the evolution of the internal physical parameters of a set of three particular fast halo CMEs. These CMEs were launched between 15 and 18 July 2002. Surprisingly, the related interplanetary CMEs (ICMEs), observed near Earth, have a low, and in one case a very low, plasma density.nMethod: We use the EUropean Heliospheric FORecasting Information Asset (EUHFORIA) model to simulate the propagation of the CMEs in the background solar wind by placing virtual spacecraft along the Sun-Earth line. We set up the initial conditions at 0.1 au, first with a cone model and then with a linear force-free spheromak model.nResults: Relatively good agreement between the simulation results and observations concerning the speed, density and arrival times of the ICMEs is obtained by adjustment of the initial CME parameters. In particular, this is achieved by increasing the initial magnetic pressure so that a fast expansion is induced in the inner heliosphere. This resulted in the development of fast expansion for two of the three ICMEs. In contrast, the intermediate ICME is strongly overtaken by the last ICME, so its expansion is strongly limited.
Czech name
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Czech description
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Classification
Type
J<sub>imp</sub> - Article in a specialist periodical, which is included in the Web of Science database
CEP classification
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OECD FORD branch
10308 - Astronomy (including astrophysics,space science)
Result continuities
Project
<a href="/en/project/GA22-10775S" target="_blank" >GA22-10775S: Analysis of plasma waves and dust grain impacts observed by RPW-TDS instrument on the Solar Orbiter spacecraft</a><br>
Continuities
I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace
Others
Publication year
2022
Confidentiality
S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů
Data specific for result type
Name of the periodical
Advances in Space Research
ISSN
0273-1177
e-ISSN
1879-1948
Volume of the periodical
70
Issue of the periodical within the volume
6
Country of publishing house
GB - UNITED KINGDOM
Number of pages
21
Pages from-to
1663-1683
UT code for WoS article
000838599300010
EID of the result in the Scopus database
2-s2.0-85134759095