2015/04/30 by Benjamin T. Lewis, Matthew R. Bate, Daniel J. Price · 2 citations
Physics and Astronomy · #Astro and Planetary Science #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Computational physics #Field (mathematics) #Magnetic field #Magnetohydrodynamic drive #Magnetohydrodynamics #Physics #Rotation (mathematics) #Smoothed-particle hydrodynamics #Stellar, planetary, and galactic studies #astro-ph.SR
paper · pdf · doi:10.1093/mnras/stv957
published as MNRAS (July 21, 2015) 451 (1): 288-299; Erratum: MNRAS (January 11, 2017) 464 (2): 2499-2501 · Accepted for publication in MNRAS, 13 pages, 14 figures. Animations can be found at http://www.astro.ex.ac.uk/people/blewis/research/outflows_misaligned_fields.html
arxiv created 2015/04/30 · openalex publication_date 2015/05/27 · arxiv updated 2018/03/29 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We have developed a modified form of the equations of smoothed particle magnetohydrodynamics which are stable in the presence of very steep density gradients. Using this formalism, we have performed simulations of the collapse of magnetized molecular cloud cores to form protostars and drive outflows. Our stable formalism allows for smaller sink particles (< 5 au) than used previously and the investigation of the effect of varying the angle, ϑ, between the initial field axis and the rotation axis. The nature of the outflows depends strongly on this angle: jet-like outflows are not produced at all when ϑ > 30°, and a collimated outflow is not sustained when ϑ > 10°. No substantial outflows of any kind are produced when ϑ > 60°. This may place constraints on the geometry of the magnetic field in molecular clouds where bipolar outflows are seen.