The magma ocean concept was first conceived to explain the geology of the Moon, but hemispherical or global oceans of silicate melt could be a widespread "lava world" phase of rocky planet accretion, and could persist on planets on short-period orbits around other stars. The formation and crystallization of magma oceans could be a defining stage in the assembly of a core, origin of a crust, initiation of tectonics, and formation of an atmosphere. The last decade has seen significant advances in our understanding of this phenomenon through analysis of terrestrial and extraterrestrial samples, planetary missions, and astronomical observations of exoplanets. This review describes the energetic basis of magma oceans and lava worlds and the lava lake analogs available for study on Earth and Io. It provides an overview of evidence for magma oceans throughout the Solar System and considers the factors that control the rocks these magma oceans leave behind. It describes research on theoretical and observed exoplanets that could host extant magma oceans and summarizes efforts to detect and characterize them. It reviews modeling of the evolution of magma oceans as a result of crystallization and evaporation, the interaction with the underlying solid mantle, and the effects of planetary rotation. The review also considers theoretical investigations on the formation of an atmosphere in concert with the magma ocean and in response to irradiation from the host star, and possible end-states. Finally, it describes needs and gaps in our knowledge and points to future opportunities with new planetary missions and space telescopes to identify and better characterize lava worlds around nearby stars.

Lava Worlds: From Early Earth to Exoplanets

Sampling of lunar regolith with a deep fluted auger: Experimental study on sampling performance

Reachability-Based Approach for Search and Detection of Maneuvering Cislunar Objects

The magma ocean concept was first conceived to explain the geology of the Moon, but hemispherical or global oceans of silicate melt could be a widespread “lava world” phase of rocky planet accretion, and could persist on planets on short-period orbits around other stars. The formation and crystallization of magma oceans could be a defining stage in the assembly of a core, origin of a crust, initiation of tectonics, and formation of an atmosphere. The last decade has seen significant advances in our understanding of this phenomenon through analysis of terrestrial and extraterrestrial samples, planetary missions, and astronomical observations of exoplanets. This review describes the energetic basis of magma oceans and lava worlds and the lava lake analogs available for study on Earth and Io. It provides an overview of evidence for magma oceans throughout the Solar System and considers the factors that control the rocks these magma oceans leave behind. It describes research on theoretical and observed exoplanets that could host extant magma oceans and summarizes efforts to detect and characterize them. It reviews modeling of the evolution of magma oceans as a result of crystallization and evaporation, the interaction with the underlying solid mantle, and the effects of planetary rotation. The review also considers theoretical investigations on the formation of an atmosphere in concert with the magma ocean and in response to irradiation from the host star, and possible end-states. Finally, it describes needs and gaps in our knowledge and points to future opportunities with new planetary missions and space telescopes to identify and better characterize lava worlds around nearby stars.

Lava worlds: From early earth to exoplanets

Advances in Drill-Based Sampling Technology for Extraterrestrial Bodies

Scientific goals, current status and nearest plans for Russian Landers missions with Luna-25 (project Luna-Glob) and Luna-27 (project Luna-Resource) will be presented. Both projects aimed on search for volatiles and water ice in upper layer of regolith, study structure and content of regolith and investigate of Moon&#8217;s near-surface dust and plasma exosphere at lunar polar regions.The scientific experiments which were selected in accordance to the main goals of these missions, will be described. Main and spare landing sites for Luna-25 will be presented selected on the base both of engineering suitability (flatness and roughness of surface, radio visibility, solar irradiation and so on) and of scientific motivation. Criteria for landing sites selection for Luna-27 will be discribed shortly too. The plan of surface operations during the first lunar days for Luna-25 and Luna-27 will be presented and discussed.The content of international cooperation for Luna-25 and Luna-27 missions will be described.It will be shown that Luna-25 and Luna-27 shell provide the necessary scientific and technological ground for future long life-time Landers at the Moon polar regions.

Russian Lunar Landers Luna-25 and Lna-27: goals of the missions and scientific investigations at Moon Polar Regions

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Russian Lunar Landers Luna-25 and Lna-27: goals of the missions and scientific investigations at Moon Polar Regions