Time-Dependent Photoionization in a Dusty Medium II: Evolution of Dust Distributions and Optical Opacities

Details Time-Dependent Photoionization in a Dusty Medium II: Evolution of Dust Distributions and Optical Opacities Time-Dependent Photoionization in a Dusty Medium II: Evolution of Dust Distributions and Optical Opacities

2002-11-12

arxiv.org/abs/astro-ph/0211235v2

Astronomy and Astrophysics

Astrophysics

ApJ in press; corrected typo in Fig.2

Scientific paper

10.1086/346109

The interaction of a radiation field with a dusty medium is a relevant issue in several astrophysical contexts. We use the time-dependent photoionization code in a dusty medium developed by Perna & Lazzati (2002), to study the modifications in the dust distribution and the relative optical opacities when a strong X-ray UV radiation flux propagates into a medium. We find that silicates are preferentially destroyed with respect to graphite, and the extinction curve becomes significantly flatter (hence implying less reddening), with the characteristic bump at lambda 2175 A highly suppressed, due to the destruction of the small graphite grains. This could explain the observational lack of such a feature in GRB afterglow and AGN spectra. For a very intense and highly variable source irradiating a compact and dense region, time variability in the optical opacity resulting from dust destruction can be observed on a relatively short timescale. We show that, under these circumstances, monitoring the time variability of the opacity can yield powerful clues on the properties of dust in the environment of the source. In particular, it allows to break the observational degeneracy as to whether a grey extinction is the result of a low dust-to-gas ratio or of a dust grain distribution that is skewed towards large grains.

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