Influence of asymmetries in the magnetic draping pattern at Titan on the emission of energetic neutral atoms

Kabanovic, S.; Feyerabend, M.; Simon, Sven; Meeks, Zachary; Wulms, Veit

doi:10.1016/j.pss.2017.12.017

Cited by 10 publications

(103 citation statements)

References 44 publications

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“…The resulting increase in λ (compared to the north) is rather subtle and completely disappears at initial ion energies around 100 keV (bottom three rows of Figure ). We note that a similar effect of the draped fields on energetic ion dynamics has been identified at Saturn's moon Titan; see discussion of Figure in Kabanovic et al ().…”

Section: Model Results: Accessibility Of Europa's Surface To Energetisupporting

confidence: 80%

“…Therefore, our particle tracing model does not require inclusion of a full model of Jupiter's magnetospheric field. Instead, we shall adapt the approach of Regoli et al (), Kabanovic et al (), and Liuzzo et al () who treated the electromagnetic fields outside of the hybrid simulation domain as spatially constant (using the upstream values from AIKEF).…”

Section: Model Descriptionmentioning

confidence: 99%

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Energetic Ion Dynamics in the Perturbed Electromagnetic Fields Near Europa

et al. 2019

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We model the dynamics of energetic magnetospheric ions in the perturbed electromagnetic fields near Jupiter's moon Europa. The inhomogeneities in the fields near Europa are generated by the induced dipole field from the moon's subsurface ocean as well as the Alfvénic plasma interaction with its ionosphere and induced field. Inhomogeneities in Europa's ionosphere at various length scales generate substantial asymmetries in the mass loading process that further complicate the structure of the moon's electromagnetic environment. In our study, the electromagnetic fields near Europa are obtained from an established hybrid model, whereas a particle tracing tool is applied to analyze the precipitation of the three most abundant energetic ion species (hydrogen, oxygen, and sulfur) onto the moon's surface at various energies from 1 keV up to 5 MeV. To isolate the contributions of the induced dipole and ionospheric mass loading to the field perturbations and the resulting precipitation patterns, we consider multiple field configurations of successively increasing complexity. For ion energies in the kiloelectron volt regime, magnetic field line draping effectively shields large portions of Europa's surface against energetic ion impacts and drastically alters the shape of the precipitation patterns, compared to uniform fields. The fine structure of these patterns strongly depends on the complexity of the applied ionosphere model. Only in the megaelectron volt regime, the precipitation patterns are qualitatively similar for uniform and draped fields. However, the precipitation of megaelectron volt ions onto Europa is still not homogeneous, since the strong magnetospheric field keeps ion gyroradii much smaller than the moon's radius.

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Section: Model Results: Accessibility Of Europa's Surface To Energetisupporting

confidence: 80%

Section: Model Descriptionmentioning

confidence: 99%

Energetic Ion Dynamics in the Perturbed Electromagnetic Fields Near Europa

et al. 2019

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“…ENA model predictions for Callisto should be extended to various plasma conditions and to ENA species other than hydrogen. ENA emissions generated by parent ion species other than hydrogen are apparently negligible at Titan (Kabanovic et al., 2018; Wulms et al., 2010) but this should be reassessed for the case of the Galilean moons before the arrival of JUICE. Including the putative Callisto neutral torus in ENA models would also allow to optimize PEP operations planning.…”

Section: Plans and Recommendationsmentioning

confidence: 99%

“…So far, ENA emissions around Callisto have never been modeled. To give an impression of the hydrogen ENA emission morphology expected at Callisto in this overview study, we have combined the draped electromagnetic fields calculated by the AIKEF hybrid model (Liuzzo et al., 2015, 2016, 2017, 2018, 2019a, 2019b) with the ENA emission model originally developed for Titan (Kabanovic et al., 2018). We consider the upstream conditions from setup # three of Liuzzo et al.…”

Section: Science Goals and Opportunities For Pep Observationsmentioning

confidence: 99%

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Callisto's Atmosphere and Its Space Environment: Prospects for the Particle Environment Package on Board JUICE

Galli

Vorburger

Mogan

et al. 2022

Earth and Space Science

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Callisto is often perceived as a boring and archaic satellite when compared to its seemingly more exciting neighbors: Io is the most volcanically active body in the solar system (Lopes, 2014 and references therein), Europa harbors a global subsurface ocean with features conducive to biology (Hand et al., 2009 and references therein), and Ganymede is the only known satellite in the solar system to possess an intrinsic magnetic field (Kivelson et al., 1996). Moreover, Io and Europa have extremely young surfaces, and Ganymede has many diverse terrains and landforms. In contrast, images of Callisto taken during Voyager flybys revealed a surface sculpted by impacts, making it the most heavily cratered Galilean satellite (Smith, Soderblom, Johnson, et al., 1979;Smith, Soderblom, Beebe, et al., 1979) and one of the oldest surfaces in the solar system. This implied that Callisto's surface was devoid of any active endogenic processes. The stigma of Callisto being an old, frozen, and geologically dead moon persisted until Galileo revealed that it is home to several exciting processes and yet unresolved mysteries of its own. For example, high-resolution images of Callisto taken by Galileo showed a surprisingly near absence of small craters on the surface, implying that, contrary to the aforementioned assumptions made about Callisto's endogenic activity, small crater degradation processes are occurring (Moore et al., 1999). Moore et al. (1999) demonstrated that these features were a result of sublimation-driven landform modification and mass wasting, and suggested Callisto possessed the most degraded surface of the icy Galilean satellites. A recent investigation by Stephan et al. (2020) of the size-distribution of water ice particles on the surface underlined the importance of temperature-driven processes for the physical properties of Callisto's surface, similar to its inner neighbor Ganymede.Although Callisto and Ganymede are of similar size and bulk composition, there are several dichotomies between the two bodies that make for an interesting comparison. While the surface of Ganymede features more diverse and complex terrains (Schenk, 1995), the surface of Callisto, in addition to being the oldest and most heavily

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