Evolution of dust grains through a hot gaseous halo

Details Evolution of dust grains through a hot gaseous halo Evolution of dust grains through a hot gaseous halo

Nov 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991apj...381..137f&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 381, Nov. 1, 1991, p. 137-146.

Astronomy and Astrophysics

Astrophysics

63

Cosmic Dust, Galactic Evolution, Halos, Interstellar Matter, Grains, Graphite, Interstellar Gas, Milky Way Galaxy, Silicates, Spiral Galaxies

Scientific paper

The evolution of bare graphite and silicate dust grains exposed to the halo environment of spiral galaxies is investigated. The evolutionary tracks are found to depend mainly on the optical properties of dust compounds because the velocities define the final fate of the grains. Graphites move faster than silicates, but both types of grains can reach values over 100 km/s. The efficiency of grain destruction increases with increasing halo gas temperature, decreasing galaxy mass, and decreasing radiation pressure coefficients. Thus, silicates behave as a 'fragile' grain population in low-mass galaxies with a hot corona. For a central halo gas density of 0.1/cu cm, spherical silicates with an initial radius of 10 exp -5 cm lose almost 20 percent of their mass on time scales between 10 exp 8 and 2 x 10 exp 8 yr.

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