Extent of the Magnetotail of Venus From the Solar Orbiter, Parker Solar Probe and BepiColombo Flybys
The result's identifiers
Result code in IS VaVaI
<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F68378289%3A_____%2F24%3A00599128" target="_blank" >RIV/68378289:_____/24:00599128 - isvavai.cz</a>
Result on the web
<a href="https://agupubs.onlinelibrary.wiley.com/doi/10.1029/2024JA032603" target="_blank" >https://agupubs.onlinelibrary.wiley.com/doi/10.1029/2024JA032603</a>
DOI - Digital Object Identifier
<a href="http://dx.doi.org/10.1029/2024JA032603" target="_blank" >10.1029/2024JA032603</a>
Alternative languages
Result language
angličtina
Original language name
Extent of the Magnetotail of Venus From the Solar Orbiter, Parker Solar Probe and BepiColombo Flybys
Original language description
We analyze data from multiple flybys by the Solar Orbiter, BepiColombo, and Parker Solar Probe (PSP) missions to study the interaction between Venus' plasma environment and the solar wind forming the induced magnetosphere. Through examination of magnetic field and plasma density signatures we characterize the spatial extent and dynamics of Venus' magnetotail, focusing mainly on boundary crossings. Notably, we observe significant differences in boundary crossing location and appearance between flybys, highlighting the dynamic nature of Venus' magnetotail. In particular, during Solar Orbiter's third flyby, extreme solar wind conditions led to significant variations in the magnetosheath plasma density and magnetic field properties, but the increased dynamic pressure did not compress the magnetotail. Instead, it is possible that the increased EUV flux at this time rather caused it to expand in size. Key findings also include the identification of several far downstream bow shock (BS), or bow wave, crossings to at least 60 RV ${mathrm{R}}_{V}$ (1 RV ${mathrm{R}}_{V}$ = 6,052 km is the radius of Venus), and the induced magnetospheric boundary to at least similar to ${sim} $ 20 RV ${mathrm{R}}_{V}$. These crossings provide insight into the extent of the induced magnetosphere. Pre-existing models from Venus Express were only constrained to within similar to ${sim} $ 5 RV ${mathrm{R}}_{V}$ of the planet, and we provide modifications to better fit the far-downstream crossings. The new model BS is now significantly closer to the central tail than previously suggested, by about 10 RV ${mathrm{R}}_{V}$ at 60 RV ${mathrm{R}}_{V}$ downstream.
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
2024
Confidentiality
S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů
Data specific for result type
Name of the periodical
Journal of Geophysical Research-Space Physics
ISSN
2169-9380
e-ISSN
2169-9402
Volume of the periodical
129
Issue of the periodical within the volume
10
Country of publishing house
US - UNITED STATES
Number of pages
17
Pages from-to
e2024JA032603
UT code for WoS article
001321297500001
EID of the result in the Scopus database
2-s2.0-85205374994