Dust Coagulation in Infalling Protostellar Envelopes. I. Compact Grains

Open Access
Publisher Website
Google Scholar
Abstract
Dust plays a key role in the optical, thermodynamic, and gasdynamical behavior of collapsing molecular cores. Because of relative velocities of the individual dust grains, coagulation and shattering can modify the grain size distribution and—because of corresponding changes in the medium's opacity—significantly influence the evolution during early phases of star formation. In order to study relevant timescales and possible consequences for intermediate-mass stars, we examine the dust evolution in spherical protostellar envelopes that evolve from cloud clumps of masses 3, 5, and 10 M☉. At first the collapse proceeds in the well-known nonhomologous manner until a central hydrostatic core is formed. During the non-steady state accretion the accretion luminosity of the central core reaches high values (≈104 L☉). Thus, differential radiative acceleration provides an important contribution to the relative velocities of the grains. In turn, the mass accretion rate, which determines the central core's accretion luminosity (and ultimately the final mass of the central object), depends strongly on the opacity distribution in the enshrouding envelope. We find that coagulation and shattering can lead to significant modifications of the dust size distribution and the opacity during early collapse phases. The visible and ultraviolet extinction is most strongly affected.