Europlanet Science Congress 2021
Virtual meeting
13 – 24 September 2021
Europlanet Science Congress 2021
Virtual meeting
13 September – 24 September 2021

OPS2

Icy worlds: Past and future explorations

The exploration of the outer solar system by Galileo at Jupiter, Cassini-Huygens at Saturn, New Horizons at Pluto-Charon and Dawn at Ceres, has revealed that several icy worlds harbor subsurface salty liquid reservoirs underneath their cold surface. By flying through the icy-vapor plume erupting from Enceladus' south pole, Cassini proceeded for the first time to the analysis of fresh materials coming from an extraterrestrial ocean, revealing its astrobiological potentials. Even if there is no direct evidence yet, similar oceanic habitats might also be present within Europa, Ganymede, Titan and Triton, which will be characterized by future missions currently under development (JUICE, Europa Clipper, Dragonfly), or under study (Europa Lander, Trident, Enceladus orbiter/lander mission). Understanding these icy ocean worlds and their connections with smaller icy moons and rings requires input from a variety of scientific disciplines: planetary geology and geophysics, atmospheric physics, life sciences, space weathering, as well as supporting laboratory studies, numerical simulations, preparatory studies for future missions and technology developments in instrumentation and engineering. We welcome abstracts that span this full breadth of disciplines required for the characterization and future exploration of icy world systems.

Co-organized by MITM
Convener: Gabriel Tobie | Co-conveners: Carly Howett, Alice Lucchetti, Frank Postberg, Federico Tosi

Session assets

Discussion on Slack

Oral and Poster presentations and abstracts

Chairpersons: Alice Lucchetti, Gabriel Tobie, Federico Tosi
EPSC2021-537
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ECP
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solicited
Luis Gomez Casajus, Marco Zannoni, Paolo Tortora, Ryan Park, Dustin Buccino, Marzia Parisi, Steven Levin, and Scott Bolton

Abstract

The Juno Extended Mission (EM) presents the first opportunity to acquire gravity measurements of the Galilean satellites after the Galileo mission, ended almost 20 years ago. On June 7th, 2021, Juno will flyby Ganymede with a closest approach altitude of ~1050km and a relative velocity of ~18.5 km/sec. This will be the first time that a probe acquires gravity measurements of Ganymede since December 28th, 2000, when Galileo performed G29, its last flyby of this Galilean moon.

In total, the Galileo probe performed 6 flybys of Ganymede, among which only 4 had coherent two-way S-band Doppler tracking during the closest approach, and could be used to estimate the gravity field of Ganymede. The very first analysis of these data, used only two flybys, G1 and G2, and estimated J2 and C22 applying the hydrostatic equilibrium constraint (J2/C22 = 10/3) (Anderson et al., 1996). The analysis concluded that Ganymede’s internal structure is likely formed by a metallic core surrounded by a silicate mantle enclosed by an ice shell. A subsequent gravity field analysis was unable to fit all tracking data (G1, G2, G7 and G29) without including a high degree gravity field nor obtain a physical interpretation of the results (Schubert et al., 2004). These problems could be solved only by adding mass anomalies to the dynamical model of Ganymede’s interior (Anderson et al., 2004; Palguta et al., 2006).

This new encounter, (G34), during Juno’s EM, offers the possibility of improving the knowledge on the gravity field of Ganymede. The gravity field of a body can be estimated through the reconstruction of the probe’s trajectory during a close encounter, exploiting the dynamical Doppler shift of a highly stable microwave carrier, induced by the relative motion between the DSN stations on the Earth and the probe. During G34, through which Juno will also perform a radio occultation experiment, the spacecraft will use simultaneously the X/X and X/Ka radio links. An accurate range-rate noise budget led us to the conclusion that we can expect an accuracy of 0.025 mm/s, at 60 s integration time, compatible to the accuracy acquired during PJ13 and PJ27, where the same radio link configuration was adopted. By comparison, the Galileo range-rate data had an accuracy of 0.34 mm/s, because of the use of S-band link and the onboard Low Gain Antenna. Moreover, this link configuration allows to use the multi-frequency link calibration technique to remove the downlink plasma contribution, preventing biases from local dispersive noises as the possible Ganymede’s ionosphere or the Io plasma torus.

Nevertheless, our results from a covariance analysis indicate that, by itself, G34 cannot provide an improvement to the current knowledge on Ganymede’s interior structure, being only able to constraint the hydrostatic ratio J2/C22 to the ~45%. This is mainly due to the flyby characteristics, and in particular the high relative velocity. However, a joint analysis with the coherent S-band radio tracking data of the Galileo spacecraft (Figure 1), acquired more than 2 decades ago, represents an opportunity to shed some light on the gravity field of this Galilean satellite.

Preliminary results from numerical simulations, performed using JPL’s orbit determination program, MONTE (Evans et al., 2018), using a setup similar to the one used for Jupiter’s gravity determination (Durante et al., 2020), indicates that the hydrostatic ratio J2/C22 could be constrained to within ~10% (1-sigma).

Figure 1: Juno and Galileo ground-tracks over Ganymede during the different encounters. The ticks are separated by 60 s.

This work will present an updated gravity field of Ganymede, showing the possible implications in terms of interior modelling. This will be the outcome of a joint analysis of all the available real data acquired during G34 and the Galileo flybys, applying modern orbit determination techniques used in the past in the Cassini gravity analyses (Durante et al., 2019, Zannoni et al., 2020). The real data used in this analysis will be the last gravity measurements of Ganymede acquirable until future flybys, of Juice and Europa Clipper missions, in the next decade.

Acknowledgements

LGC, MZ and PT are grateful to the Italian Space Agency (ASI) for financial support through Agreement No. 2017-40-H.0, and its extension 2017-40-H.1-2020, for ESA’s BepiColombo and NASA’s Juno radio science experiments. The work of RP, DB, MP, and SL was carried out at the Jet Propulsion Lab, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Government sponsorship acknowledged.

References

  • Anderson, J. D., Lau, E. L., Sjogren, W. L., Schubert, G., & Moore, W. B. (1996). Gravitational constraints on the internal structure of Ganymede. Nature, 384(6609), 541-543.
  • Anderson, J. D., Schubert, G., Jacobson, R. A., Lau, E. L., Moore, W. B., & Palguta, J. L. (2004). Discovery of mass anomalies on Ganymede. Science, 305(5686), 989-991.
  • Durante, D., Hemingway, D. J., Racioppa, P., Iess, L., & Stevenson, D. J. (2019). Titan's gravity field and interior structure after Cassini. Icarus, 326, 123-132.
  • Durante, D., Parisi, M., Serra, D., Zannoni, M., Notaro, V., Racioppa, P., ... & Bolton, S. J. (2020). Jupiter's gravity field halfway through the Juno mission. Geophysical Research Letters, 47(4), e2019GL086572.
  • Evans, S., Taber, W., Drain, T., Smith, J., Wu, H. C., Guevara, M., ... & Evans, J. (2018). MONTE: The next generation of mission design and navigation software. CEAS Space Journal, 10(1), 79-86.
  • Palguta, J., Anderson, J. D., Schubert, G., & Moore, W. B. (2006). Mass anomalies on Ganymede. Icarus, 180(2), 428-441.
  • Schubert, G., Anderson, J. D., Spohn, T., & McKinnon, W. B. (2004). Interior composition, structure and dynamics of the Galilean satellites. Jupiter: The planet, satellites and magnetosphere, 1, 281-306.
  • Zannoni, M., Hemingway, D., Casajus, L. G., & Tortora, P. (2020). The gravity field and interior structure of Dione. Icarus, 345, 113713.

How to cite: Gomez Casajus, L., Zannoni, M., Tortora, P., Park, R., Buccino, D., Parisi, M., Levin, S., and Bolton, S.: The gravity field of Ganymede after the Juno Extended Mission, Europlanet Science Congress 2021, online, 13–24 Sep 2021, EPSC2021-537, https://doi.org/10.5194/epsc2021-537, 2021.

EPSC2021-329
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ECP
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solicited
Gianluca Chiarolanza, Giuseppe Mitri, and Monica Pondrelli

Introduction: Chaotic terrains on the icy moon Europa are among the youngest surface features within the satellite’s visible geological history [1]. These regions appear as highly disrupted surfaces formed by irregular groups of isolated plates surrounded by a lumpy matrix material [2]. They are often covered in a reddish-brown material that is interpreted to consist of hydrated sulfates [3] or sulfuric acid hydrate [4]. Current models of chaos formation include a melt-through of the surface provoked by an internal heat source (i.e. a hydrothermal plume) [5], or the mobilization of brines trapped near the surface, in response to partial melting of the outer shell induced by icy diapirs rising through the crust [6]. We investigated two chaotic terrains named Thrace Macula and Thera Macula, both located on the southern hemisphere of Europa. Among the hypotheses proposed to explain their origin are the upwarping of the surface followed by an extrusion of low-viscosity liquids [7, 8], the collapse of large-scale domes [9], or interactions between the ice and shallow subsurface water lenses [10]. Here we provide a geomorphological and stratigraphic analysis of Thrace and Thera Macula, derived from an extensive geological mapping based on the highest-resolution images of the area acquired throughout the Galileo space mission. We also provide preliminary results of a topographic analysis performed on photoclinometric DEMs obtained using Ames Stereo Pipeline [11, 12].

 

Figure 1. Geological Map of Thrace (right) and Thera Macula (left).

 

Results: The mapped area includes plains dominated by ridge complexes, bands, linear features (double ridges, troughs), craters (for less than 1%), and chaotic terrains (Fig. 1). Local displacements of band margins and double ridges suggest the occurrence of crustal movements along tectonic faults.

Thera Macula is characterized by a distinctive dichotomy between its northern, partly fractured icy plain, and the southern complex of low-albedo chaotic terrains. The margins of the macula, particularly to the north, appear heavily fractured and forming a complex of steep scarps faced towards the macula, with elevations ranging from -30 to -390 m (Fig. 2). The southern lobe is the only one displaying a positive relief up to 360 m in height. The dark, chaotic terrain consists for 85% of matrix material, and for 15% of large plates that show signs of displacement. On average, plates rise up to 320 m from the surrounding matrix, and some can exceed 700 m in height. Apparently, the matrix has replaced a pre-existing terrain which underwent a strong degradation process.

Thrace Macula exhibits a larger proportion of matrix material, which makes up to 98% of the macula’s surface, while the remaining 2% is composed of blocks. The latter are represented either by large plates not completely detached from the margins (only identified in the northern sector), or by small sub-kilometer, often tilted blocks found in the center of the macula. In contrast to Thera, the boundaries are not marked by steep scarps, and the matrix looks domed up above the surrounding plain. The macula’s northern and central sectors are separated by a bright, roughly linear stripe that could be an intersecting double ridge postdating the formation of the macula. The high-resolution images of the southern lobe show the presence of a higher-albedo matrix, where any pre-existing structure is no longer recognizable, and a lower-albedo matrix, where the pre-existing features are still preserved and appear mostly unaltered.