This work describes the scientific process that transformed the pioneering empirical solution of jet grouting into an engineering technique. In its basic version, jet grouting involves drilling small holes in the ground and emitting jets of cement grout at very high speed while extracting and rotating the drill rods, to cut the soil, mix it with the binder and form cemented columns. The dimensions and mechanical properties of the columns depend on the ability of the jet to disintegrate the original soil fabric, mix particles and mortar homogeneously, and carry out the cement reaction. In this process the hydrodynamics of submerged turbulent jets play a fundamental role. Observation and theory intertwine to analyze, conceptualize, and simulate basic mechanisms. The result is a closed-form relationship, simple but complete, capable of capturing the role of the fundamental factors. Aim of this process is to reduce the subjectivity and uncertainties inherent in the applications and pave the way for the improvement of the technique. Finally, a practical application is reported to show the potential of the scientific approach on improving the technique.

In the scientific field of collisionless shocks, interplanetary space comprises a critical natural laboratory allowing the study of processes at spatial scales which are impossible to recreate in laboratories on Earth. Despite decades of research, key questions in the dynamics of collisionless shocks including energy transport and exchange remain unresolved due to instrumental limitations. With the return of humanity to the Moon and the upcoming construction of the Lunar Platform: Gateway (LOP-G) space station, the possibility arises to study the pristine solar wind in unprecedented detail, with the space station potentially enabling significant power capacity and data rates which would be challenging to achieve on smaller unmanned spacecraft. The space station's location in a lunar halo orbit allows the study of the solar wind away from the contaminating influence of the terrestrial bow shock. Here we propose to utilize nitrogen-vacancy (NV) diamond technology to combine magnetometer, temperature and plasma density measurements into a single instrument which can sample kHz-range magnetic field with sensitivities on the order of <1e-5 nT, while also sounding the local plasma density and temperature. These capabilities will generate datasets which will contribute significantly to shock science, helping answer key outstanding questions in the field. Simultaneously, these observations will improve understanding of space weather dynamics, contribute to cross-calibrating complementary missions, and probe the lunar exosphere. With the paucity of long-term, high-cadence, high-sensitivity pristine solar wind datasets, the Diamond Experiment In the MagnetOSphere (DEIMOS) will fill a key need for the solar wind and collisionless shocks community.

The circumlunar environment is a dusty plasma consisting of small particles of lunar regolith, photoelectrons, electrons, and solar wind ions. When moving around the Earth, part of the trajectory of the Moon passes through the Earth's magnetosphere. In addition, the magnetic field is characteristic for some areas on the Moon, the so-called lunar magnetic anomalies. The magnetic field values above these areas can exceed the magnetic field values of the Earth's magnetosphere in the region of the Moon's trajectory by one or two orders of magnitude. The magnetic field and photoelectron density gradients can lead to the development of drift turbulence. The relevant conditions are discussed in this work.

The introduction of cloud condensation nuclei and radiative heating by sunlight-absorbing aerosols can modify the thickness and coverage of low clouds, yielding significant radiative forcing of climate. The magnitude and sign of changes in cloud coverage and depth in response to changing aerosols are impacted by turbulent dynamics of the cloudy atmosphere, but integrated measurements of aerosol solar absorption and turbulent fluxes have not been reported thus far. Here we report such integrated measurements made from unmanned aerial vehicles (UAVs) during the CARDEX (Cloud Aerosol Radiative Forcing and Dynamics Experiment) investigation conducted over the northern Indian Ocean. The UAV and surface data reveal a reduction in turbulent kinetic energy in the surface mixed layer at the base of the atmosphere concurrent with an increase in absorbing black carbon aerosols. Polluted conditions coincide with a warmer and shallower surface mixed layer because of aerosol radiative heating and reduced turbulence. The polluted surface mixed layer was also observed to be more humid with higher relative humidity. Greater humidity enhances cloud development, as evidenced by polluted clouds that penetrate higher above the top of the surface mixed layer. Reduced entrainment of dry air into the surface layer from above the inversion capping the surface mixed layer, due to weaker turbulence, may contribute to higher relative humidity in the surface layer during polluted conditions. Measurements of turbulence are important for studies of aerosol effects on clouds. Moreover, reduced turbulence can exacerbate both the human health impacts of high concentrations of fine particles and conditions favorable for low-visibility fog events.

The Acceleration, Reconnection, Turbulence, and Electrodynamics of the Moon's Interaction with the Sun (ARTEMIS) mission is a spin-off from NASA's Medium-class Explorer (MIDEX) mission THEMIS, a five identical micro-satellite (hereafter termed probe) constellation in high altitude Earth-orbit since 17 February 2007. By repositioning two of the five THEMIS probes (P1 and P2) in coordinated, lunar equatorial orbits, at distances of similar to 55-65 R (E) geocentric (similar to 1.1-12 R (L) selenocentric), ARTEMIS will perform the first systematic, two-point observations of the distant magnetotail, the solar wind, and the lunar space and planetary environment. The primary heliophysics science objectives of the mission are to study from such unprecedented vantage points and inter-probe separations how particles are accelerated at reconnection sites and shocks, and how turbulence develops and evolves in Earth's magnetotail and in the solar wind. Additionally, the mission will determine the structure, formation, refilling, and downstream evolution of the lunar wake and explore particle acceleration processes within it. ARTEMIS's orbits and instrumentation will also address key lunar planetary science objectives: the evolution of lunar exospheric and sputtered ions, the origin of electric fields contributing to dust charging and circulation, the structure of the lunar interior as inferred by electromagnetic sounding, and the lunar surface properties as revealed by studies of crustal magnetism. ARTEMIS is synergistic with concurrent NASA missions LRO and LADEE and the anticipated deployment of the International Lunar Network. It is expected to be a key element in the NASA Heliophysics Great Observatory and to play an important role in international plans for lunar exploration.

NASA's two spacecraft ARTEMIS mission will address both heliospheric and planetary research questions, first while in orbit about the Earth with the Moon and subsequently while in orbit about the Moon. Heliospheric topics include the structure of the Earth's magnetotail; reconnection, particle acceleration, and turbulence in the Earth's magnetosphere, at the bow shock, and in the solar wind; and the formation and structure of the lunar wake. Planetary topics include the lunar exosphere and its relationship to the composition of the lunar surface, the effects of electric fields on dust in the exosphere, internal structure of the Moon, and the lunar crustal magnetic field. This paper describes the expected contributions of ARTEMIS to these baseline scientific objectives.