2007/09/30 by Kaitlin M. Kratter, Christopher D. Matzner, Mark R. Krumholz +1 · 3 citations
Materials Science · Physics and Astronomy · #Accretion (finance) #Angular momentum #Astro and Planetary Science #Astrophysics and Star Formation Studies #Chemical and Physical Properties of Materials #Dimensionless quantity #Gravitational instability #Protostar #Star formation #Stars #Stellar evolution #astro-ph
paper · pdf · doi:10.1086/587543
17 pages, 9 figures, accepted for publication in ApJ. Model updated to better reflect simulations in the literature; discussion of key assumptions and strategy clarified
arxiv created 2008/02/12 · openalex publication_date 2008/07/01 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/06
Most analytic work to date on protostellar disks has focused on those in isolation from their environments. However, observations are now beginning to probe the earliest, most embedded phases of star formation, during which disks are rapidly accreting from their parent cores and cannot be modeled in isolation. We present a simple, one-zone model of protostellar accretion disks with high-mass infall rates. Our model combines a self-consistent calculation of disk temperatures with an approximate treatment of angular momentum transport via two mechanisms. We use this model to survey the properties of protostellar disks across a wide range of stellar masses and evolutionary times and make predictions for disks' masses, sizes, spiral structure, and fragmentation that will be directly testable by future large-scale surveys of deeply embedded disks. We define a dimensionless accretion-rotation parameter that, in conjunction with the disk's temperature, controls the disk evolution. We track the dominant mode of angular momentum transport and demonstrate that for stars with final masses greater than roughly one solar mass, gravitational instabilities are the most important mechanism as most of the mass accumulates. We predict that binary formation through disk fission, fragmentation of the disk into small objects, and spiral arm strength all increase in importance to higher stellar masses.