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Habitable zones around main sequence stars.
The results suggest that mid-to-early K stars should be considered along with G stars as optimal candidates in the search for extraterrestrial life. Expand
Simulations of the Atmospheres of Synchronously Rotating Terrestrial Planets Orbiting M Dwarfs: Conditions for Atmospheric Collapse and the Implications for Habitability☆
Abstract Planets within the habitable zones of M dwarfs are likely to be synchronous rotators; in other words, one side is permanently illuminated while the other side is in perpetual darkness. WeExpand
Melting of Io by Tidal Dissipation
The dissipation of tidal energy in Jupiter's satellite Io is likely to have melted a major fraction of the mass. Consequences of a largely molten interior may be evident in pictures of Io's surfaceExpand
Thermal histories, compositions and internal structures of the moons of the solar system
Thermal evolution models of satellites are discussed with emphasis placed on the fundamental physical processes common to all planetary bodies. A comparison is made between the different evolutionaryExpand
Interactions of planetesimals with protoplanetary atmospheres
Abstract We compute the interaction of planetesimals with the envelopes of growing giant planets that form by the “core-instability” mechanism. According to this mechanism, a core grows by theExpand
Pioneer Venus gas chromatography of the lower atmosphere of Venus
A gas Chromatograph mounted in the Pioneer Venus sounder probe measured the chemical composition of the atmosphere of Venus at three altitudes. Ne, N2, O2, Ar, CO, H2O, SO2, and CO2 were measured,Expand
The evolution of Enceladus
Saturn's small icy moon Enceladus shows evidence of several episodes of geologic resurfacing and extensional tectonism spread over much of its history. Freezing of liquid in the interior causedExpand
Liquid water and active resurfacing on Europa
Voyager images of the jovian moon Europa show a bright icy surface transected by a complex pattern of long, linear fracture-like markings with a slightly lower albedo1. Very few impact craters areExpand
Tidal dissipation, orbital evolution, and the nature of Saturn's inner satellites
Abstract Estimates of tidal damping times of the orbital eccentricities of Saturn's inner satellites place constraints on some satellite rigidities and dissipation functions Q . These constraintsExpand
A slightly more massive young Sun as an explanation for warm temperatures on early Mars.
The valley network channels on the heavily cratered ancient surface of Mars suggest the presence of liquid water approximately 3.8 Gyr ago. However, the implied warm climate is difficult to explainExpand