New Images of Europa from Juno’s JunoCam

Post contributed by Dr Candice J. Hansen, Planetary Science Institute, USA

On the 29th of September 2022 the Juno spacecraft, in orbit around Jupiter, made a close pass by Jupiter’s icy moon Europa (Image 1). The spacecraft approached from Europa’s night side, passed the terminator (day-night boundary), and departed on the day side, coming within ~350 km of the surface.  Juno’s visible color imager, JunoCam, snapped 4 images of Europa as the spacecraft sped by at a speed of 23.6 km/sec on its way to its closest approach to Jupiter.  In an elliptical polar orbit, this was the only opportunity in the mission for Juno to get close to this moon of Jupiter and the first time since the Galileo mission ended in 2003 that any spacecraft has flown so close. 

Image 1.  The first image taken by JunoCam is centered on the subjovian hemisphere, extending to ~60 deg north and south.  This was the highest resolution image acquired. Image data: NASA/JPL-Caltech/SwRI/MSSS. Image processing: Brian Swift © CC BY.

Europa is categorized as an “ocean world” with a solid ice surface over a liquid water subsurface layer.  Europa is crisscrossed by numerous cracks, bands, ridges and troughs (lineaments) that record the tidal stress the moon experiences arising from the gravitational pull of Jupiter and its other moons. JunoCam’s image reveals numerous pits along the terminator.  The almost complete lack of craters tells us that geologically this icy surface is very young, resurfaced by lineament formation due to tidal flexing.  Callanish crater, one of the few imaged by JunoCam, is the circular feature visible in the lower right of Image 1.  

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Chaotic Terrain on Pluto, Europa, and Mars

Post contributed by Helle L. Skjetne, PhD candidate, Department of Earth and Planetary Sciences, University of Tennessee, Knoxville, USA.

Chaos terrain is formed by disruption of preexisting surfaces into irregularly shaped blocks with a “chaotic” appearance (Image 1). This typically occurs through fracturing (that can be induced by a variety of mechanisms), and the subsequent evolution of these blocks can follow several paths (Image 2). These distinctive areas of broken terrains are most notably found on Jupiter’s moon Europa, Mars, and Pluto. Although chaos terrains on these bodies share some common characteristics, there are also distinct morphological differences between them (Image 1). The geologic evolution required to shape this enigmatic terrain type has not yet been fully constrained, although several chaos formation models have been proposed. We studied chaotic terrain blocks on Pluto, Europa and Mars to infer information about crustal lithology and surface layer thickness (Skjetne et al. 2020).

Image 1: Examples of chaotic terrain “blocks” (referring to each mountain-like topographic feature). Chaos on Pluto in a) Tenzing Montes and b) Al-Idrisi Montes, respectively (New Horizons image at ~315 m px–1), c) Hydraotes Chaos on Mars (Mars Odyssey THEMIS daytime infrared global mosaic at 100 m px–1), and d) Conamara Chaos on Europa (Galileo 210–220 m px–1 East and West RegMaps).

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