Extent of the Magnetotail of Venus From the Solar Orbiter, Parker Solar Probe and BepiColombo Flybys

Kód výsledku v 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>

Výsledek na webu

<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>

Jazyk výsledku

angličtina

Název v původním jazyce

Extent of the Magnetotail of Venus From the Solar Orbiter, Parker Solar Probe and BepiColombo Flybys

Popis výsledku v původním jazyce

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.

Název v anglickém jazyce

Extent of the Magnetotail of Venus From the Solar Orbiter, Parker Solar Probe and BepiColombo Flybys

Popis výsledku anglicky

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.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

<a href="/cs/project/GA22-10775S" target="_blank" >GA22-10775S: Analýza plazmových vln a dopadů prachových částic pozorovaných přístrojem RPW-TDS na sondě Solar Orbiter</a><br>

Návaznosti

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Rok uplatnění

2024

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

2169-9402

Svazek periodika

129

Číslo periodika v rámci svazku

10

Stát vydavatele periodika

US - Spojené státy americké

Počet stran výsledku

17

Strana od-do

e2024JA032603

Kód UT WoS článku

001321297500001

EID výsledku v databázi Scopus

2-s2.0-85205374994