Toggle Main Menu Toggle Search

Open Access padlockePrints

The supernova-regulated ISM III. Generation of vorticity, helicity, and mean flows

Lookup NU author(s): Fred Gent, Dr Graeme Sarson

Downloads


Licence

This is the final published version of an article that has been published in its final definitive form by EDP Sciences, 2018.

For re-use rights please refer to the publisher's terms and conditions.


Abstract

The forcing of interstellar turbulence, driven mainly by supernova explosions, is irrotational in nature, but the development of significant amounts of vorticity and helicity, accompanied by large-scale dynamo action, has been reported. Several earlier investigations examined vorticity production in simpler systems; here all the relevant processes can be considered simultaneously. We also investigate the mechanisms for the generation of net helicity and large-scale flow in the system. We use a three-dimensional, stratified, rotating and shearing local simulation domain of the size 1x1x2 kpc3, forced with SN explosions occurring at the rate typical of the solar neighbourhood in the Milky Way. In addition to the nominal simulation run with realistic Milky Way parameters, we vary the rotation and shear rates, but keep the absolute value of their ratio fixed. Reversing the sign of shear vs. rotation allows us to separate the rotation- and shear-generated contributions. As in earlier studies, we find the generation of significant amounts of vorticity, with on average 65% of the kinetic energy being in the rotational modes. The vorticity production can be related to the baroclinicity of the flow, especially in the regions of hot, dilute clustered supernova bubbles. In these regions, the vortex stretching acts as a sink of vorticity. The net helicities produced by rotation and shear are of opposite signs for physically motivated rotation laws, with the solar neighbourhood parameters resulting in the near cancellation of the total net helicity. We also find the excitation of oscillatory mean flows, the strength and oscillation period of which depend on the Coriolis and shear parameters; we interpret these as signatures of the anisotropic kinetic (AKA) effect. We use the method of moments to fit for the turbulent transport coeffcients, and find αAKA values of the order 3-5 km/s.


Publication metadata

Author(s): Käpylä MJ, Gent FA, Väisälä MS, Sarson GR

Publication type: Article

Publication status: Published

Journal: Astronomy and Astrophysics

Year: 2018

Volume: 611

Online publication date: 20/03/2018

Acceptance date: 09/10/2017

Date deposited: 18/10/2017

ISSN (print): 0004-6361

ISSN (electronic): 1432-0746

Publisher: EDP Sciences

URL: https://doi.org/10.1051/0004-6361/201731228

DOI: 10.1051/0004-6361/201731228


Altmetrics

Altmetrics provided by Altmetric


Actions

Find at Newcastle University icon    Link to this publication


Share