Mantle formation, coagulation, and the origin of cloud/core shine
I. Modelling dust scattering and absorption in the infrared
Institut d’Astrophysique Spatiale, CNRS, Univ. Paris-Sud, Université
2 School of Physics and Astronomy, Queen Mary, University of London, 327 Mile End Road, London, E1 4NS, UK
3 Centre de Sciences Nucléaires et de Sciences de la Matière, UMR 8609, CNRS/Université Paris Sud, Université Paris-Saclay, Université Paris Sud, 91405 Orsay, France
Received: 1 October 2015
Accepted: 1 February 2016
Context. The observed cloudshine and coreshine (C-shine) have been explained in terms of grain growth leading to enhanced scattering from clouds in the J, H, and K photometric bands and the Spitzer IRAC 3.6 and 4.5 μm bands.
Aims. Using our global dust-modelling approach THEMIS (The Heterogeneous dust Evolution Model at the IaS), we explore the effects of dust evolution in dense clouds, through aliphatic-rich carbonaceous mantle formation and grain-grain coagulation.
Methods. We model the effects of wide band gap a-C:H mantle formation and the low-level aggregation of diffuse interstellar medium dust in the moderately-extinguished outer regions of molecular clouds.
Results. The formation of wide band gap a-C:H mantles on amorphous silicate and amorphous carbon (a-C) grains leads to a decrease in their absorption cross-sections but no change in their scattering cross-sections at near-infrared wavelengths, resulting in higher albedos.
Conclusions. The evolution of dust, with increasing density and extinction in the diffuse-to-dense molecular cloud transition, through mantle formation and grain aggregation, appears to be a likely explanation for the observed C-shine.
Key words: dust, extinction / ISM: general / evolution
© ESO, 2016