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dc.contributor.authorKociscak, Samuel
dc.contributor.authorKvammen, Andreas
dc.contributor.authorMann, Ingrid Brigitte
dc.contributor.authorMeyer-Vernet, Nicole
dc.contributor.authorPisa, David
dc.contributor.authorSouček, Jan
dc.contributor.authorTheodorsen, Audun
dc.contributor.authorVaverka, Jakub
dc.contributor.authorZaslavsky, Arnaud
dc.date.accessioned2024-05-30T07:11:30Z
dc.date.available2024-05-30T07:11:30Z
dc.date.issued2024-05-29
dc.description.abstractSolar Orbiter is equipped with electrical antennas performing fast measurements of the surrounding electric field. The antennas register high-velocity dust impacts through the electrical signatures of impact ionization. Although the basic principle of the detection has been known for decades, the understanding of the underlying process is not complete, due to the unique mechanical and electrical design of each spacecraft and the variability of the process.<p> <p>We present a study of electrical signatures of dust impacts on Solar Orbiter's body, as measured with the Radio and Plasma Waves electrical suite. A large proportion of the signatures present double-peak electrical waveforms in addition to the fast pre-spike due to electron motion, which are systematically observed for the first time. We believe this is due to Solar Orbiter's unique antenna design and a high temporal resolution of the measurements. The double peaks are explained as being due to two distinct processes. Qualitative and quantitative features of both peaks are described. The process for producing the primary peak has been studied extensively before, and the process for producing the secondary peak has been proposed before (Pantellini et al., 2012a) for Solar Terrestrial Relations Observatory (STEREO), although the corresponding delay of 100–300 µs between the primary and the secondary peak has not been observed until now.<p> <p>Based on this study, we conclude that the primary peak's amplitude is the better measure of the impact-produced charge, for which we find a typical value of around 8 pC. Therefore, the primary peak should be used to derive the impact-generated charge rather than the maximum. The observed asymmetry between the primary peaks measured with individual antennas is quantitatively explained as electrostatic induction. A relationship between the amplitude of the primary and the secondary peak is found to be non-linear, and the relation is partially explained with a model for electrical interaction through the antennas' photoelectron sheath.en_US
dc.identifier.citationKociscak, Kvammen, Mann, Meyer-Vernet, Pisa, Souček, Theodorsen, Vaverka, Zaslavsky. Impact ionization double peaks analyzed in high temporal resolution on Solar Orbiter. Annales Geophysicae. 2024;42(1):191-212en_US
dc.identifier.cristinIDFRIDAID 2271631
dc.identifier.doi10.5194/angeo-42-191-2024
dc.identifier.issn0992-7689
dc.identifier.issn1432-0576
dc.identifier.urihttps://hdl.handle.net/10037/33647
dc.language.isoengen_US
dc.publisherEuropean Geosciences Union (EGU)en_US
dc.relation.ispartofKočiščák, S. (2024). Understanding Inner Solar System Dust Environment Through In-Situ Measurements. (Doctoral thesis). <a href=https://hdl.handle.net/10037/34747>https://hdl.handle.net/10037/34747</a>
dc.relation.journalAnnales Geophysicae
dc.rights.accessRightsopenAccessen_US
dc.rights.holderCopyright 2024 The Author(s)en_US
dc.rights.urihttps://creativecommons.org/licenses/by/4.0en_US
dc.rightsAttribution 4.0 International (CC BY 4.0)en_US
dc.titleImpact ionization double peaks analyzed in high temporal resolution on Solar Orbiteren_US
dc.type.versionpublishedVersionen_US
dc.typeJournal articleen_US
dc.typeTidsskriftartikkelen_US
dc.typePeer revieweden_US


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Attribution 4.0 International (CC BY 4.0)
Med mindre det står noe annet, er denne innførselens lisens beskrevet som Attribution 4.0 International (CC BY 4.0)