Influence of Europa’s Time‐Varying Electromagnetic Environment on Magnetospheric Ion Precipitation and Surface Weathering

Addison, Peter; Liuzzo, Lucas; Arnold, H. J. P.; Simon, Sven

doi:10.1029/2020ja029087

Cited by 24 publications

(194 citation statements)

References 101 publications

(470 reference statements)

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“…Thus, while the Alfvén wings generate a protective "envelope" around Europa that partially shields the surface from the impinging plasma, the additional protection rendered by ramside field pile-up was shown to be far weaker than hypothesized by preceding studies (e.g., Paranicas et al, 2000). Therefore, the findings of Addison et al (2021) imply that the results presented in this section can be considered a very reasonable approximation to emulate ion precipitation onto Europa at equatorial latitudes.…”

Section: Number Flux Of Magnetospheric Plasmamentioning

confidence: 54%

Role of the Ionospheric Conductance Profile in Sub‐Alfvénic Moon‐Magnetosphere Interactions: An Analytical Model

2021

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The Galilean moons of Jupiter and the largest satellites of Saturn are located within their parent planets' magnetospheres where they are continuously overtaken by a partially corotating plasma flow. The obstacle that a moon represents to this incident magnetospheric plasma can consist mainly of its dense atmosphere and ionosphere, as is the case at Jupiter's volcanic moon Io (Blöcker et al., 2018) and Saturn's largest moon Titan (e.g., Neubauer et al., 1984, 2006Simon et al., 2015). At Europa, Ganymede, and Callisto the resulting ionosphere-magnetosphere interaction is modified to a varying degree by permanent or induced magnetic moments from the objects' interiors and ionospheres (e.g.

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Section: Number Flux Of Magnetospheric Plasmamentioning

confidence: 54%

Role of the Ionospheric Conductance Profile in Sub‐Alfvénic Moon‐Magnetosphere Interactions: An Analytical Model

2021

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“…4 of 27 the energetic particle environments near the moons of Jupiter (Addison et al, 2021;Breer et al, 2019;Liuzzo et al, 2019aLiuzzo et al, , 2019bLiuzzo et al, , 2020 and Saturn (Kotova et al, 2015;Krupp et al, 2020;Regoli et al, 2016), reaching agreement with spacecraft measurements. The hybrid approach in general, and the AIKEF model in particular, is therefore well suited to study the plasma interaction of Triton.…”

Section: 1029/2021ja029740mentioning

confidence: 55%

“…By doing so, we constrain two representative scenarios of Triton's interaction with Neptune's magnetospheric plasma. as denoted by the outlined red star in Figure 1) would generate plasma signatures that are qualitatively similar to those for the case of 𝐴𝐴 𝐴𝐴= 47 • (see also, e.g., Addison et al, 2021;. We therefore do not investigate the scenario with 𝐴𝐴 𝐴𝐴= 133 • here.…”

Section: Triton's Magnetospheric Plasma Environmentmentioning

confidence: 92%

“…We use a power law to extrapolate this spectrum up to 10 MeV, consistent with the electron energies present within Neptune's magnetosphere (Krimigis et al, 1989;Mauk et al, 1991). Note that while Triton's perturbed electromagnetic environment likely affects the resulting electron precipitation and ionization patterns (e.g., Addison et al, 2021;Liuzzo et al, 2019aLiuzzo et al, , 2019bRegoli et al, 2016), we assume that electrons precipitate isotropically onto Triton's atmosphere as a first order approximation (see also Liuzzo et al, 2015).…”

Section: Triton's Atmosphere and Ionospherementioning

confidence: 97%

“…However, the plasma interaction in turn affects the structure of Triton's induced magnetic field, similar to the interaction at Jupiter's moons Europa or Callisto (see, e.g., Arnold et al, 2019;Blöcker et al, 2016;Harris et al, 2021;Schilling et al, 2008;Liuzzo et al, 2015): pileup of the local magnetic field compresses the induced field at the ramside hemisphere, while convection stretches it toward downstream. Despite this interaction, the Galileo spacecraft detected distinct signatures of the nearly unaltered induced fields at Callisto and Europa within a narrow region located near these moons' wakeside surfaces (Arnold, Liuzzo, & Simon, 2020;Addison et al, 2021;Liuzzo et al, 2016). It is therefore possible that a similar region where signatures of the "pure" inductive response, shielded from effects of the plasma interaction, also exists near Triton.…”

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confidence: 99%

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Triton’s Variable Interaction With Neptune’s Magnetospheric Plasma

et al. 2021

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Neptune's largest moon Triton (radius 𝐴𝐴 𝐴𝐴𝑇𝑇 = 1, 353 km) is thought to be an erstwhile Kuiper belt object that was captured by the ice giant (Agnor & Hamilton, 2006). Orbiting at a radial distance of 𝐴𝐴 14.4𝑅𝑅𝑁𝑁 (radius of Neptune 𝐴𝐴 𝐴𝐴𝑁𝑁 = 24, 622 km), Triton is always located within Neptune's magnetosphere (Curtis & Ness, 1986;Mejnertsen et al., 2016;Ness et al., 1989;Richardson, 1993). The moon's highly inclined orbit-tilted nearly 𝐴𝐴 157 • with respect to its parent planet's rotational equator-results in a retrograde orbital motion around Neptune. Triton possesses the second-most dense moon atmosphere in the solar system after Titan (Broadfoot et al., 1989;Strobel et al., 1990;Strobel & Zhu, 2017). Mainly comprised of neutral 𝐴𝐴 N2 , its maximum surface number density is on the order of 𝐴𝐴 10 15 cm −3 , with a scale height between 10 and 70 km (Broadfoot et al., 1989). Additionally, trace gases including methane are present, with surface densities below 𝐴𝐴 10 11 cm −3 (e.g., Summers & Strobel, 1991;Trafton, 1984;Krasnopolsky et al., 1992). This neutral envelope is predominantly ionized by a combination of magnetospheric electron impacts and photoionization, resulting in an ionospheric Pedersen conductance that may exceed 𝐴𝐴 10 4 S (Strobel et al., 1990). In addition to this global atmosphere, observations during the Voyager 2 encounter of Neptune in 1989 indicated localized, geyser-like vapor plumes emanating from the surface to an altitude of ∼10 km (Smith et al., 1989). Since the moon's interior is likely differentiated in a hydrosphere and rocky mantle, it is possible that these plumes originate from a global, deep ocean sustained via radiogenic heating and/or tidal forcing (Nimmo & Spencer, 2015).

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Investigating Europa’s Radiation Environment with the Europa Clipper Radiation Monitor

Meitzler,

Jun,

Blase

et al. 2023

Space Sci Rev

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We present an overview of the radiation environment monitoring program planned for the Europa Clipper mission. The harsh radiation environment of Jupiter will be measured by a dedicated Radiation Monitor (RadMon) subsystem, yielding mission accumulative Total Ionizing Dose (TID) and instantaneous electron flux measurements with a 1-Hz cadence. The radiation monitoring subsystem is comprised of a stand alone sensor assembly along with distributed TID assemblies at various locations on the spacecraft. The sensor assembly itself is made of a TID sensor stack using the Metal-Oxide Semiconducting Field-Effect Transistor (MOSFET) and a Charge Rate Monitor (CRM) that uses a stack of bulk charge collection plates. The TID measurements will provide the critical information about the overall radiation levels relevant to the degradation of electronics over time, and the electron flux data can serve as a proxy for the Internal ElectroStatic Discharge (IESD) environment by measuring the >∼1 MeV electron environment. In addition, the radiation monitoring subsystem data will be augmented by serendipitous radiation data from science instruments onboard. This will be enabled by careful modeling and analysis of opportunistic background data from potentially the following instruments: Europa Imaging System (EIS), Europa-Ultraviolet Spectrograph (Europa-UVS), Mapping Imaging Spectrometer for Europa (MISE), MAss Spectrometer for Planetary EXploration (MASPEX), Plasma Instrument for Magnetic Sounding (PIMS), and SUrface Dust Analyzer (SUDA). Based on the current analysis, these instruments will be most sensitive to >1 MeV electrons. As such, the high-energy electron data obtained by the radiation monitoring subsystem will be qualitatively and quantitatively enhanced by the high-energy electron data acquired by the instruments. The holistic radiation monitoring program for the mission will be an extensive collaboration among many teams across the flight and payload systems.Although the radiation monitoring subsystem itself is an engineering resource for the mission, the collective data from the mission can also be used to improve the scientific understanding of the Jovian magnetosphere and the high-energy electron environment near Europa, where the motion of charged particles is perturbed by the local electromagnetic environment. The data could also help in the understanding of the radiation modification of Europa surface compounds, which could subsequently help guide lab experiments to aid in understanding the origin and evolution of surface materials and in constraining the interpretation of observational data. To this end, the radiation monitoring subsystem is a useful resource for helping address the Europa Clipper mission’s primary goal of assessing the habitability of Europa.

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Influence of Europa’s Time‐Varying Electromagnetic Environment on Magnetospheric Ion Precipitation and Surface Weathering

Cited by 24 publications

References 101 publications

Role of the Ionospheric Conductance Profile in Sub‐Alfvénic Moon‐Magnetosphere Interactions: An Analytical Model

Role of the Ionospheric Conductance Profile in Sub‐Alfvénic Moon‐Magnetosphere Interactions: An Analytical Model

Triton’s Variable Interaction With Neptune’s Magnetospheric Plasma

Investigating Europa’s Radiation Environment with the Europa Clipper Radiation Monitor

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