Impact of the Hall effect in star formation : improving the angular momentum conservation

Abstract

We present here a minor modification of our numerical implementation of the Hall effect for the 2D Riemann solver used in Constrained Transport schemes, as described in Marchand et al. (2018). In the previous work, the tests showed that the angular momentum was not conserved during protostellar collapse simulations, with significant impact. By removing the whistler waves speed from the characteristic speeds of non-magnetic variables in the 1D Riemann solver, we are able to improve the angular momentum conservation in our test-case by one order of magnitude, while keeping the second-order numerical convergence of the scheme. We also reproduce the simulations of Tsukamoto et al. (2015) with consistent resistivities, the three non-ideal MHD effects and initial rotation, and agree with their results. In this case, the violation of angular momentum conservation is negligible in regard to the total angular momentum and the angular momentum of the disk.

6 pages, 6 figures, published in A&A

References in corpus (2)

• The impact of the Hall effect during cloud core collapse:implications for circumstellar disk evolution
• The impact of non-ideal magnetohydrodynamics on binary star formation

Cited by in corpus (5)

• Formation and Evolution of Disks around Young Stellar Objects
• Protostellar collapse: the conditions to form dust rich protoplanetary disks
• Hall Effect in Protostellar Disc Formation and Evolution
• The impact of non-ideal magnetohydrodynamic processes on discs, outflows, counter-rotation and magnetic walls during the early stages of star formation
• Do we need non-ideal magnetohydrodynamics to model protostellar discs?