The Jupiter and Icy Moons Explorer (JUICE) mission of the European Space Agency (ESA) will investigate the Jovian system with multiple instruments over several years, beginning in early 2031. This paper describes the historical context and state of knowledge, as well as JUICE’s scientific goals and measurement techniques of the satellites that will not be encountered in close flybys. These include the large volcanically active moon Io, the four small inner moons Metis, Adrastea, Amalthea, and Thebe, and the numerous small Irregular (outer) moons. JUICE will provide multiple opportunities to observe Io from relatively remote distances of hundreds of thousands of kilometers. These observations will enable monitoring of Io’s surface for changes, and for the study of its neutral clouds and plasma torus. Io observations will be performed with the four optical remote sensing instruments and with the Particle Environment Package. For the small inner moons it is planned to obtain complete geographic longitude (scales up to 8 km/px), solar-phase and multi-color coverage, oblique polar views, and UV to near-IR spectra. Astrometric measurements will also be performed. The Irregular moons will mostly appear unresolved to the JUICE instruments. Nonetheless, long-duration disk-integrated lightcurves will be acquired to derive rotation periods, object dimensions, pole-axis orientations, and colors for most objects for the first time. From these data, convex-shape models will be generated and phase curves determined. Furthermore, the precision of the orbital elements will be improved via accurate astrometry. UV and near-IR measurements will be attempted for the largest of these objects.

For future integration of a large number of qubits and complementary metal-oxide-semiconductor (CMOS) controllers, higher operation temperature of qubits is strongly desired. In this work, we fabricate p-channel silicon quantum dot (Si QD) devices on silicon-on-insulator for strong confinement of holes and investigate the temperature dependence of Coulomb oscillations and Coulomb diamonds. The physically defined Si QDs show clear Coulomb diamonds at temperatures up to 25 K, much higher than for gate defined QDs. To verify the temperature dependence of Coulomb diamonds, we carry out simulations and find good agreement with the experiment. The results suggest a possibility for realizing quantum computing chips with qubits integrated with CMOS electronics operating at higher temperature in the future.

Observations obtained with the near-infrared camera NIRC2, coupled to the adaptive optics system on the 10-m W.M. Keck II telescope on Mauna Kea, Hawaii, on 14 August 2007 revealed an active and highly-energetic eruption at Pillan at 245.2±0.7°W and 8.5±0.5°S. A one-temperature blackbody fit to the data revealed a (blackbody) temperature of 840±40K over an area of 17km², with a total power output of ~500GW. Using Davies' (Davies, A.G. [1996]. Icarus 124(1), 45-61) Io Flow Model, we find that the oldest lava present is less than 1-2h old, having cooled down from the eruption temperature of >1400K to ~710K; this young hot lava suggests that an episode of lava fountaining was underway. In addition to an examination of this eruption, we present data of the Pele and Pillan volcanoes obtained with the same instrument and telescope from 2002 through 2015. These data reveal another eruption at Pillan on UT 28 June 2010. Model fits to this eruption yield a blackbody temperature of 600-700K over an area of ~60km², radiating over 600GW. On UT 18 February 2015 an energetic eruption was captured by the InfraRed Telescope Facility (IRTF) via mutual event occultations. The eruption took place at 242.7±1°W and 12.4±1°S, i.e., in the eastern part of Pillan Patera. Subsequent observations showed a gradual decrease in the intensity of the eruption. Images obtained with the Keck telescope on 31 March and 5 May 2015 revealed that the locations of the eruption had shifted by 120-160km to the NW.In contrast to the episodicity of Pillan, Pele has been persistent, observed in every appropriate 4.7μm observation. Pele was remarkably consistent in its thermal emission from the Galileo era through February 2002, when a blackbody temperature of 940±40K and an area of 6.5km² was measured. Since that time, however, the radiant flux from what is likely a apparently large, overturning lava lake has gradually subsided over the next decade by a factor of ~4, while the location of the thermal source was moving back and forth between areas roughly ~100km to the W of the 2002 location and an area roughly ~100km to the SE of the 2002 location.