2015/09/16 by Geoffroy Lesur, P. Hennebelle, Patrick Hennebelle +2 · 59 citations
Physics and Astronomy · #Accretion (finance) #Amplitude #Angular momentum #Astro and Planetary Science #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Classical mechanics #Inflow #Mechanics #Physics #RADIUS #Shock wave #Specific relative angular momentum #Spiral (railway) #Spiral galaxy #Stars #Stellar, planetary, and galactic studies #Total angular momentum quantum number #astro-ph.SR
paper · pdf · doi:10.1051/0004-6361/201526734
published in Astronomy and Astrophysics 582, L9 (EDP Sciences) · 4 pages, 4 figures, accepted in A&A Letters
arxiv created 2015/09/16 · openalex publication_date 2015/09/28 · arxiv updated 2015/10/14 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We numerically investigate the dynamics of a 2D non-magnetised protoplanetary disc surrounded by an inflow coming from an external envelope. We find that the accretion shock between the disc and the inflow is unstable, leading to the generation of large-amplitude spiral density waves. These spiral waves propagate over long distances, down to radii at least ten times smaller than the accretion shock radius. We measure spiral-driven outward angular momentum transport with 10-4 ≲ α < 10-2 for an inflow accretion rate Ṁinf ≳ 10-8 M⊙ yr-1. We conclude that the interaction of the disc with its envelope leads to long-lived spiral density waves and radial angular momentum transport with rates that cannot be neglected in young non-magnetised protostellar discs.