title: On the evolution and activity of cometary nuclei.
abstract: The thermal evolution of a spherical cometary nucleus (initial radius of 2.5 km), composed initially of very cold amorphous ice and moving in comet Halley's orbit, is simulated numerically for 280 revolutions.  It is found that the phase transition from amorphous to crystalline ice constitutes a major internal heat source.  The transition does not occur continuously, but in five distinct rounds, during the following revolutions: 1, 7, 40-41, 110-112, and 248-252.  Due to the (slow) heating of the amorphous ice between crystallization rounds, the phase transition front advances into the nucleus to progressively greater depths:  36 m on the first round, and then 91 m, 193 m, 381 m, and 605 m respectively.  Each round of crystallization starts when when the boundary between amorphous and crystalline ice is brought to approximately 15 m below the surface, as the nucleus radius decreases due to sublimation.  At the time of crystallization, the temperature of the transformed ice rises to 180 K.  According to experimental studies of gas-laden amorphous ice, a large fraction of the gas trapped in the ice at low temperatures is released.  Whereas some of the released gas may find its way out through cracks in the crystalline ice layer, the rest is expected to accumulate in gas pockets that may eventually explode, forming "volcanic calderas."  The gas-laden amorphous ice thus exposed may be a major source of gas and dust jets into the coma, such as those observed on comet Halley by the Giotto spacecraft.  The activity of new comets and, possibly, cometary outbursts and splits may also be explained in terms of explosive gas release following the transition from amorphous to crystalline ice.
authors.affiliation: Department of Geophysics and Planetary Sciences, Tel-Aviv University.
authors.forename: D
authors.initials: D
authors.lastname: Prialnik
authors.forename: A
authors.initials: A
authors.lastname: Bar-Nun
mesh_terms: D003460:Crystallization; D019419:Evolution, Planetary; D005740:Gases; D007053:Ice; D008433:Mathematics; D019110:Meteoroids; D008956:Models, Chemical; D013696:Temperature
chemical_list: D005740:Gases; D007053:Ice