Magma oceans in the inner solar system

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Thermal evolution of an early magma ocean in interaction with the atmosphere (2012, unknown): “For the volatile content used in the calculation of Marcq [2012], the threshold temperature is around 2000 K.”
Origin and evolution of the atmospheres of early Venus, Earth and Mars (2018, methodology): “…adiabatic temperature profile that likely characterizes a turbulent and well-mixed magma ocean is steeper than the slopes of the liquidus and solidus, the solidification of a magma ocean likely begins at its bottom and proceeds upwards (e.g. Walker et al. 1975; Solomatov 2000; Elkins-Tanton 2012).”
Melting and differentiation of early-formed asteroids: The perspective from high precision oxygen isotope studies (2017, background): “…Mars and Earth, all of which had protracted high- temperature evolutions (e.g. Warren, 1985; Tonks and Melosh, 1993; Rubie et al., 2004; Wood et al., 2006; Halliday and Wood, 2010; Elkins-Tanton, 2012) demonstrates that isotopic homogenization was extremely efficient on these much smaller bodies.”
Evidence for multiple magma ocean outgassing and atmospheric loss episodes from mantle noble gases (2013, background): “Global magma oceans are thought to be a natural result of the highly energetic giant impact phase of planetary accretion (Abe and Matsui, 1985; Benz and Cameron, 1990; Canup, 2008; Elkins-Tanton, 2012; Sasaki and Nakazawa, 1986; Stevenson, 1987; Tonks and Melosh, 1993).”