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Impact of the transport of magnetospheric electrons on the composition of the Triton atmosphere

hal.structure.identifierLaboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
hal.structure.identifierASP 2024
dc.contributor.authorBENNE, B.
hal.structure.identifierLaboratoire de Physique Atmosphérique et Planétaire [LPAP]
dc.contributor.authorBENMAHI, B.
hal.structure.identifierASP 2024
dc.contributor.authorDOBRIJEVIC, Michel
hal.structure.identifierASP 2024
hal.structure.identifierPôle Planétologie du LESIA
hal.structure.identifierLaboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics [LESIA]
dc.contributor.authorCAVALIÉ, Thibaut
hal.structure.identifierInstitut des Sciences Moléculaires [ISM]
dc.contributor.authorLOISON, Jean-Christophe
hal.structure.identifierInstitut des Sciences Moléculaires [ISM]
dc.contributor.authorHICKSON, Kevin M.
hal.structure.identifierInstitut de Planétologie et d'Astrophysique de Grenoble [IPAG]
dc.contributor.authorBARTHELEMY, Mathieu
hal.structure.identifierInstitut de Planétologie et d'Astrophysique de Grenoble [IPAG]
dc.contributor.authorLILENSTEN, Jean
dc.date.issued2024
dc.identifier.issn0004-6361
dc.description.abstractEnContext: Due to its inclined orbit and the complex geometry of the magnetic field of Neptune, Triton experiences a highly variable magnetic environment. As precipitation of magnetospheric electrons is thought to have a large impact on the Triton atmosphere, a better understanding of the interaction between its atmosphere and the magnetosphere of Neptune is important.Aims: We aim to couple a model of the Triton atmosphere with an electron transport model to compute the impact of a varying electron precipitation on the atmospheric composition.Methods: We coupled a recent photochemical model of the Triton atmosphere with the electron transport model TRANSPlanets. The inputs of this code were determined from Voyager 2 observations and previous studies. The main inputs were the electron precipitation flux, the orbital scaling factor, and the magnetic field strength. The electron-impact ionization and electron-impact dissociation rates computed by TRANSPlanets were then used in the photochemical model. We also analyzed the model uncertainties.Results: The coupling of the two models enabled us to find an electron density profile, as well as N 2 and N number densities, that are consistent with the Voyager 2 observations. We found that photoionization and electron-impact ionization are of the same order, in contrast to the results of previous photochemical models. However, we emphasize that this result depends on the hypotheses we used to determine the input variables of TRANSPlanets. Our model would greatly benefit from new measurements of the magnetic environment of Triton, as well as of the electron fluxes in the Neptune magnetosphere.
dc.language.isoen
dc.publisherEDP Sciences
dc.subject.enastrochemistry: planets and satellites
dc.subject.enatmospheres: planets and satellites
dc.subject.enplanets and satellites: magnetic fields
dc.title.enImpact of the transport of magnetospheric electrons on the composition of the Triton atmosphere
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361/202346699
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.pageA22
bordeaux.volume686
bordeaux.peerReviewedoui
hal.identifierhal-04659943
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-04659943v1
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