The goal of the Ariel space mission is to observe a large and diversified population of transiting planets around a range of host star types to collect information on their atmospheric composition. The planetary bulk and atmospheric compositions bear the marks of the way the planets formed: Ariel's observations will therefore provide an unprecedented wealth of data to advance our understanding of planet formation in our Galaxy. A number of environmental and evolutionary factors, however, can affect the final atmospheric composition. Here we provide a concise overview of which factors and effects of the star and planet formation processes can shape the atmospheric compositions that will be observed by Ariel, and highlight how Ariel's characteristics make this mission optimally suited to address this very complex problem.
Departamento de Estado Sólido, Instituto de Física, Universidad Nacional Autónoma de México, Circuito de la Investigación Científica, Ciudad Universitaria, Ciudad de México, 04510, México.
A prebiotic model, based in the framework of thermodynamic efficiency loss from small dissipative eukaryote organisms [1-3], is developed to describe the maximum possible concentration of solar power to be dissipated on topological circular molecules structures encapsulated in lipid-walled vacuoles, which floated in the Archean oceans. By considering previously, the analysis of 71 species examined by covering 18 orders of mass magnitude from the Megapteranovaeangliae to Saccharomyces cerevisiae[2], suggest that in molecular structures of smaller masses than any living being known nowadays, the power dissipation must be directly proportional to the power of the photons of solar origin that impinge them to give rise to the formation of more complex self-assembled molecular structures at the prebiotic stage by a quantum mechanics model of resonant photon wavelength excitation. The analysis of 12 circular molecules (encapsulated in lipid-walled vacuoles) relevant to the evolution of life on planet Earth such as the five nucleobases, and some aromatic molecules as pyrimidine, porphyrin, chlorin, coumarin, xanthine, etc.
Impact cratering is one of the fundamental processes throughout the history of the Solar System. The formation of new impact craters on planetary bodies has been observed with repeat images from orbiting satellites. However, the time gap between images is often large enough to preclude detailed analysis of smaller-scale features such as secondary impact craters, which are often removed or buried over a short time period.
The last giant impact on Earth is thought to have formed the Moon. The timing of this event can be determined by dating the different rocks assumed to have crystallized from the lunar magma ocean (LMO). This has led to a wide range of estimates for the age of the Moon between 4.
The possible presence of brines on Mars adds an intriguing dimension to the exploration of Martian environments. Their potential involvement in the formation of recurring slope lineae has sparked debates on the existence of liquid water versus alternative dry processes. In situ instrumentation on rovers and landers has been instrumental in providing valuable data for comprehending the dynamics of brines.
The formation of complex craters requires some form of transient weakening of target rocks. Acoustic fluidization is one proposed mechanism applied in many numerical simulations of large crater formation. In a companion paper, we describe implementing the Melosh model of acoustic fluidization in the iSALE shock physics code.
