Articles | Volume 41, issue 2
https://doi.org/10.5194/angeo-41-389-2023
© Author(s) 2023. This work is distributed under
the Creative Commons Attribution 4.0 License.
the Creative Commons Attribution 4.0 License.
https://doi.org/10.5194/angeo-41-389-2023
© Author(s) 2023. This work is distributed under
the Creative Commons Attribution 4.0 License.
the Creative Commons Attribution 4.0 License.
Regular paper
| 
10 Oct 2023
Regular paper |
| 10 Oct 2023
| 10 Oct 2023
Statistical distribution of mirror-mode-like structures in the magnetosheaths of unmagnetized planets – Part 2: Venus as observed by the Venus Express spacecraft
Space Research Institute, Austrian Academy of Sciences, Graz, Austria
Cyril Simon Wedlund
Space Research Institute, Austrian Academy of Sciences, Graz, Austria
David Mautner
Space Research Institute, Austrian Academy of Sciences, Graz, Austria
Sebastián Rojas Mata
Swedish Institute of Space Physics, Kiruna, Sweden
Gabriella Stenberg Wieser
Swedish Institute of Space Physics, Kiruna, Sweden
Yoshifumi Futaana
Swedish Institute of Space Physics, Kiruna, Sweden
Christian Mazelle
Institut de Recherche en Astrophysique et Planétologie (IRAP), Université de Toulouse, CNRS, UPS, CNES, Toulouse, France
Diana Rojas-Castillo
Instituto de Geofísica, Universidad Nacional Autónoma de México, Coyoacán, Mexico
César Bertucci
Instituto de Astronomía y Física del Espacio, Autonomous City of Buenos Aires, Argentina
Magda Delva
Space Research Institute, Austrian Academy of Sciences, Graz, Austria
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In this work we present the first analytical magnetosheath plasma flow model for the space environment around Mercury. The proposed model is relatively simple to implement and provides the possibility to trace the flow lines inside the Hermean magnetosheath. It can help to determine the the local plasma conditions of a spacecraft in the magnetosheath exclusively on the basis of the upstream solar wind parameters.
Martin Volwerk, David Mautner, Cyril Simon Wedlund, Charlotte Goetz, Ferdinand Plaschke, Tomas Karlsson, Daniel Schmid, Diana Rojas-Castillo, Owen W. Roberts, and Ali Varsani
Ann. Geophys., 39, 239–253, https://doi.org/10.5194/angeo-39-239-2021, https://doi.org/10.5194/angeo-39-239-2021, 2021
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The magnetic field in the solar wind is not constant but varies in direction and strength. One of these variations shows a strong local reduction of the magnetic field strength and is called a magnetic hole. These holes are usually an indication that there is, or has been, a temperature difference in the plasma of the solar wind, with the temperature along the magnetic field lower than perpendicular. The MMS spacecraft data have been used to study the characteristics of these holes near Earth.
Herbert Gunell, Charlotte Goetz, Elias Odelstad, Arnaud Beth, Maria Hamrin, Pierre Henri, Fredrik L. Johansson, Hans Nilsson, and Gabriella Stenberg Wieser
Ann. Geophys., 39, 53–68, https://doi.org/10.5194/angeo-39-53-2021, https://doi.org/10.5194/angeo-39-53-2021, 2021
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When the magnetised solar wind meets the plasma surrounding a comet, the magnetic field is enhanced in front of the comet, and the field lines are draped around it. This happens because electric currents are induced in the plasma. When these currents flow through the plasma, they can generate waves. In this article we present observations of ion acoustic waves, which is a kind of sound wave in the plasma, detected by instruments on the Rosetta spacecraft near comet 67P/Churyumov–Gerasimenko.
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Short summary
Freshly created ions in solar wind start gyrating around the interplanetary magnetic field. When they cross the bow shock, they get an extra kick, and this increases the plasma pressure against the magnetic pressure. This leads to the creation of so-called mirror modes, regions where the magnetic field decreases in strength and the plasma density increases. These structures help in exploring how energy is transferred from the ions to the magnetic field and where around Venus this is happening.
Freshly created ions in solar wind start gyrating around the interplanetary magnetic field. When...
