Large-scale three-dimensional numerical simulations of the deflagration stage of a thermonuclear supernova explosion show the formation and evolution of a highly convoluted turbulent flame in a gravitational field of an expanding carbon-oxygen white dwarf. The flame dynamics is dominated by the gravity-induced Rayleigh-Taylor instability that controls the burning rate. The thermonuclear deflagration releases enough energy to produce a healthy explosion. The turbulent flame, however, leaves large amounts of unburnt and partially burnt material near the star center, whereas observations imply these materials only in outer layers. This disagreement could be resolved if the deflagration triggers a detonation.

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A Monte Carlo simulation in n-butane dissolved in water shows that at 300 K water induces a dramatic shift in the conformational equilibrium of n-butane from what is observed in either the gas phase or in non-hydrogen-bonded liquids; however, at 333 K, this strong solvent effect disappears.

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