This hands-on introduction to numerical geodynamic modelling provides a solid grounding
in the necessary mathematical theory and techniques, including continuum mechanics and …

The water content of magma oceans is widely accepted as a key factor that determines
whether a terrestrial planet is habitable. Water ocean mass is determined as a result not only …

The 182Hf–182W systematics of meteoritic and planetary samples provide firm constraints
on the chronology of the accretion and earliest evolution of asteroids and terrestrial planets …

In early Solar System during the runaway growth stage of planetary formation, the
distribution of planetary bodies progressively evolved from a large number of planetesimals …

A classic scenario of core formation suggests that growing proto-planets are heated by the
impacts of accreting planetesimals at their surface until their shallow layers reach the …

Due to mechanisms such as impact heating, early atmospheric thermal blanketing, and
radioactive heating, the presence of at least one global magma ocean stage in the early …

Many innovative laboratory experiments have been used to investigate the fluid dynamics of
the Earth's core. Experiments with liquid metals and non-metals range from turbulence and …

The thermal evolution of planets during their accretionary growth is strongly influenced by
impact heating. The temperature increase following a collision takes place mostly below the …

Core formation in terrestrial planets is a complex process, possibly involving several
mechanisms. This paper presents a direct numerical simulation of one of these, the …

The transition from Newtonian to non‐Newtonian flow of silicate melts is commonly
manifested as shear thinning at conditions of high stress and strain rate. Shear thinning may …