Chemical evolution of interstellar dust, comets and the origins of life.
It now appears that the chemical evolution of the pre-solar system interstellar dust ensures that a major fraction of comets is in the form of complex organic molecules at least partially of a prebiotic nature and that the submicron interstellar dust preserves  its chemical integrity as result of forming a very tenuous low density comet structure whose solid matter occupies approximately 1/5 of the total volume.  This low density micro structure further provides a physical basis for comets bringing a significant fraction of the original interstellar organic molecules to the earth unmodified by the impact event.  Finally, the evidence for a large number of comet collisions with the early earth ensured that the major organic molecular budget on the earth's surface was "continuously" supplied along with water well before 3.8 billion years ago which is the earliest date for life.  The chemistry and morphological structure of a comet nucleus as an aggregate of interstellar dust is used to provide comparisons with a variety of comet Halley results:  the density of the nucleus and of the dust; the dust cloud model and its consequences on the production of C+ and CN in the coma by small organic grains; the surface albedo and the low nucleus heat conductivity and high surface temperature; the appearance of 10(-14) g and 10(-17) g dust particles along with higher masses; the mass spectra of dust and infrared spectroscopy as evidence for complex organic grain mantles and of very small (approximately 0.01 micrometer) carbonaceous and silicate grains; the appearance of small grains resulting from breakup of larger grains.  The cosmic ray dosage of a comet nucleus during its 4.5 billion years in the Oort cloud appears to be  many orders of magnitude less than the dosage of the preaggregated interstellar dust by ultraviolet photons except perhaps in the outer few meters of the nucleus of a new comet.  The heat conductivity calculated for aggregated dust is certainly less than 10(-4) that of crystalline ice.  This, in combination with the interstellar dust microstructure, provide a basis for showing that solar heating of the interior of a nucleus is lower than previously estimated.
Greenberg
J M
JM
Laboratory Astrophysics, University of Leiden, The Netherlands.
Zhao
N
N
Hage
J
J
D002244:Carbon / Q000032:analysis; D019443:Cosmic Dust / Q000032:analysis*; D019418:Evolution, Chemical; D005118:Extraterrestrial Environment; D019110:Meteoroids; D000069497:Origin of Life; D010316:Particle Size; D017785:Photons; D017640:Silicates / Q000032:analysis; D016082:Solar System; D013055:Spectrophotometry, Infrared
D019443:Cosmic Dust; D017640:Silicates; D002244:Carbon