The formation of small grains in shocks in the ISM

Details The formation of small grains in shocks in the ISM The formation of small grains in shocks in the ISM

May 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994dib..nasa...79j&link_type=abstract

In its The Diffuse Interstellar Bands: Contributed Papers 79-83 (SEE N95-15827 03-89)

Astronomy and Astrophysics

Astronomy

1

Carbonaceous Materials, Collisions, Destruction, Grain Size, Interplanetary Dust, Interstellar Matter, Polycyclic Aromatic Hydrocarbons, Radio Astronomy, Shock Waves, Silicates, Supernovae, Algorithms, Betatrons, Deformation, Fragmentation, Mathematical Models, Vaporizing

Scientific paper

Carbonaceous and silicate grains swept up, and betatron accelerated, by supernova-generated shock waves in the interstellar medium are exposed to grain destructive processing. The degree of grain destruction is determined by the differential gas-grain and grain-grain velocities, which lead to sputtering of the grain surface and grain core disruption (deformation, vaporization and shattering), respectively. The threshold pressure for grain shattering in grain-grain collisions (100 k bar) is considerably lower than that for vaporization (approximately 5 M bar). Therefore, collisions between grains shatter large grains into smaller fragments (i.e., small grains and PAH's). Using a new algorithms for the destructive processes, it was possible to model the formation fo small grain fragments in grain-grain collisions in the warm phase of the interstellar medium. It was found that in one cycle through the warm medium (approximately 3 x 106 years) of order 1-2% of the total grain mass is shattered into particles with radii of less than 50 A.

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