Dust Sublimation and Fragmentation in the Circumburst Medium: Evidence for a Large, Massive Cloud Origin for Gamma-Ray Bursts with Dark Optical Afterglows

The distances to which the optical flash destroys dust via sublimation, and the burst and afterglow change the size distribution of the dust via fragmentation, are functions of grain size. Furthermore, the sublimation distance is a decreasing function of grain size, while the fragmentation distance is a decreasing function of grain size for large grains and an increasing function of grain size for small grains. We investigate how these very different, but somewhat complementary, processes change the optical depth of the circumburst medium. To this end, we adopt a canonical distribution of graphite and silicate grain sizes, and a simple fragmentation model, and we compute the post-burst/optical flash/afterglow optical depth of a circumburst cloud of constant density n and size R as a function of burst and afterglow isotropic-equivalent X-ray energy E and spectral index α, and optical flash isotropic-equivalent peak luminosity L: This improves upon previous analyses that consider circumburst dust of a uniform grain size. We find that circumburst clouds do not significantly extinguish (τ ∼< 0.3) the optical afterglow if R ∼< 10L 1/2 49 pc, fairly independent of n, E, and α, or if NH ∼< 5 × 10 20 cm−2. On the other hand, we find that circumburst clouds do significantly extinguish (τ ∼> 3) the optical afterglow if R ∼> 10L 1/2 49 pc and NH ∼> 5×10 21 cm−2, creating a so-called ‘dark burst’. The majority of bursts are dark, and as circumburst extinction is probably the primary cause of this, this implies that most dark bursts occur in clouds of this size and mass M ∼> 3× 10 L49 M⊙. Clouds of this size and mass are typical of giant molecular clouds, and are active regions of star formation. Subject headings: dust, extinction — gamma rays: bursts — ISM: clouds Department of Astronomy, California Institute of Technology, Mail Code 105-24, 1201 East California Boulevard, Pasadena, CA 91125 Hubble Fellow