June 8-12, 2014


Superbubble Feedback in Galaxy Simulations

Ben Keller (McMaster University)

J. Wadsley, S.M. Benincasa, H.M.P Couchman (all of McMaster University)

We present a superbubble-based stellar feedback model. Superbubbles driven by clustered massive stars evaporate a fraction of the swept-up shells into their hot interior. We simulate superbubbles by including thermal conduction, sub-grid evaporation, and a brief multiphase treatment at lower resolutions. Previous models typically heated too much mass, producing a hot ISM below 10^6K that cools away feedback energy unless ad-hoc cooling suppression is applied. The physics of thermal conduction sets the amount of gas heated by feedback, avoiding additional free parameters. We use SPH simulations to show that this model is insensitive to resolution and can produce Milky Way and dwarf galaxy analogues with Kennicutt-Schmidt star formation rate laws and strong outflows.
(to be confirmed by the SOC)