2009/03/03 by G. Meeus, Gwendolyn Meeus, Meeus, Gwendolyn
Chemistry · Physics and Astronomy · #Astro and Planetary Science #Astrophysics and Star Formation Studies #Earth and Planetary Astrophysics (astro-ph.EP) #FOS: Physical sciences #Molecular Spectroscopy and Structure #Solar and Stellar Astrophysics (astro-ph.SR) #astro-ph.EP #astro-ph.SR
paper · pdf · doi:10.48550/arxiv.0903.0480
To appear in the proceedings of "Cosmic Dust -- Near and Far," ed. Th. Henning, E. Gruen and J. Steinacker (ASP Conf. Ser., 2009)
arxiv created 2009/03/03 · openalex publication_date 2009/03/03 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
The dust in the interstellar medium, that provides the material for forming stars - and circumstellar discs as a natural by-product - is known to have submicron sizes. As these discs are the sites of planet formation, those small grains are predicted to grow to larger entities when the stars are still young. will review evidence for the first steps in grain growth in proto-planetary discs around young stars, based on recent Spitzer and ground-based infrared observations. First, I will discuss disc and dust properties in Herbig Ae/Be stars, and then move to the lower-mass T Tauri stars and the brown dwarfs. Here, objects of different star-forming regions are compared, and the influence of the stellar parameters and environment on dust evolution, as witnessed by the observed dust characteristics, is discussed.