2010/05/01 by Dennis F. Duffin, Dennis Duffin, Ralph E. Pudritz · 1 citation
Physics and Astronomy · #Astro and Planetary Science #Astronomy and Astrophysical Research #Astrophysics and Star Formation Studies #Core (optical fiber) #Eddy current brake #Magnetic field #Magnetohydrodynamics #Protostar #Stars #Torque #Transient (computer programming) #astro-ph.GA #astro-ph.SR #physics.comp-ph
paper · pdf · doi:10.1017/s1743921311000536
published in Proceedings of the International Astronomical Union 6(S270), 291-295 (Cambridge University Press) · 5 pages, 4 figures, conference proceedings of IAU Symposium 270 (eds. Alves, Elmegreen, Girart, Trimble)
openalex publication_date 2010/05/01 · arxiv created 2010/09/22 · arxiv updated 2015/05/20 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
Abstract The pre-stellar cores in which low mass stars form are generally well magnetized. Our simulations show that early protostellar discs are massive and experience strong magnetic torques in the form of magnetic braking and protostellar outflows. Simulations of protostellar disk formation suggest that these torques are strong enough to suppress a rotationally supported structure from forming for near critical values of mass-to-flux. We demonstrate through the use of a 3D adaptive mesh refinement code – including cooling, sink particles and magnetic fields – that one produces transient 1000 AU discs while simultaneously generating large outflows which leave the core region, carrying away mass and angular momentum. Early inflow/outflow rates suggest that only a small fraction of the mass is lost in the initial magnetic tower/jet event.