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https://doi.org/10.5194/egusphere-2025-60
© Author(s) 2025. This work is distributed under
the Creative Commons Attribution 4.0 License.
the Creative Commons Attribution 4.0 License.
https://doi.org/10.5194/egusphere-2025-60
© Author(s) 2025. This work is distributed under
the Creative Commons Attribution 4.0 License.
the Creative Commons Attribution 4.0 License.
31 Jan 2025
| 31 Jan 2025
Status: this preprint is open for discussion and under review for Annales Geophysicae (ANGEO).
Ion beam instability model for the Mercury upstream waves
Abstract. An analytic model for the ion beam instability is constructed in view of application to the Mercury upstream waves. Our ion beam instability model determines the frequency and the wavenumber by equating the whistler dispersion relation with the beam resonance condition in favor of planetary foreshock wave excitation. By introducing the Doppler shift in the instability frequency, our model can derive the observer-frame relation of the resonance frequency to the beam velocity and the flow speed. The frequency relation serves as a useful diagnostic tool to the Mercury upstream wave studies in the upcoming BepiColombo observations.
How to cite. Narita, Y., Schmid, D., and Motschmann, U.: Ion beam instability model for the Mercury upstream waves, EGUsphere [preprint], https://doi.org/10.5194/egusphere-2025-60, 2025.
Publisher's note: Copernicus Publications remains neutral with regard to jurisdictional claims made in the text, published maps, institutional affiliations, or any other geographical representation in this preprint. The responsibility to include appropriate place names lies with the authors.
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Yasuhito Narita
CORRESPONDING AUTHOR
Institut für Theoretische Physik, Technische Universität Braunschweig, Mendelssohnstr. 3, D-38106 Braunschweig, Germany
Daniel Schmid
Space Research Institute, Austrian Academy of Sciences, Schmiedlstr. 6, 8042 Graz, Austria
Uwe Motschmann
Institut für Theoretische Physik, Technische Universität Braunschweig, Mendelssohnstr. 3, D-38106 Braunschweig, Germany
Short summary
It is often the case that only magnetic field data are available in in-situ planetary studies using spacecraft. Plasma data are either not available or the amount is highly limited. Nevertheless, the theory of plasma instability tells us how to interpret the magnetic field data (wave frequency) in terms of flow speed and beam velocity generating the instability. We invent an analysis tool for the Mercury upstream waves as example.
It is often the case that only magnetic field data are available in in-situ planetary studies...