A complete numerical description of galaxy formation in a cosmological
environment has still to be developed: the physical processes involved
in star formation act on scales (<1 pc) that are too small
to be resolved in simulations describing the cosmological environment
(> 1 Mpc). So, such processes need to be included in simulations
as sub-resolution effective models.
In this framework, we developed MUPPI, a sub-resolution model
for star formation and feedback, loosely based on the earlier semi-analytic
multi-phase model of the inter-stellar medium (ISM) by Monaco (2004).
- MUPPI is implemented in the Gadget code.
- The ISM evolution is described by a system of ordinary
differential equations that drives mass and energy flows among a cold
gas phase, a hot gas phase and a stellar component inside each
- The system is integrated with an adaptive Runge-Kutta integrator
within the SPH time-step
- The energy resulting from SNe is re-distributed to neighbours;
thermal energy is given to the hot phase, whose long cooling time
ensures that it is not immediately radiated away.
- Kinetic energy is distributed in a similar way to a much more limited
set of particles, so as to trigger massive outflows.
- In cosmological runs the overhead due to MUPPI is around 15%.
Physical regimes for feedback in galaxy formation,
P. Monaco, 2004, MNRAS, 352, 181,
On the destruction of
star-forming clouds, P. Monaco, 2004, MNRAS, 354, 151
A sub-resolution multiphase interstellar medium model
of star formation and SNe energy feedback,
G. Murante, P. Monaco, M. Giovalli, S. Borgani &
A. Diaferio, 2010, MNRAS, 405, 1491.
Schmidt-Kennicutt relations in SPH simulations of disc galaxies
with effective thermal feedback from supernovae,
P. Monaco, G. Murante, S. Borgani & K. Dolag, 2012, MNRAS, 421, 2485.
A Warm Mode of Gas Accretion on Forming Galaxies,
G. Murante, M Calabrese, G. De Lucia, P. Monaco, S. Borgani & K. Dolag,
2012, ApJ, 749, L34
The Aquila comparison project: the effects of feedback and numerical methods
on simulations of galaxy formation
C. Scannapieco, M. Wadepuhl, O.H. Parry et al., 2012, MNRAS, 423, 1726.
Simulating realistic disc galaxies with a novel sub-resolution ISM model,
G. Murante, P. Monaco, S. Borgani, L. Tornatore, K., Dolag & D. Goz,
2015, MNRAS, 447, 178.
Properties of barred spiral discs in hydrodynamical cosmological simulations,
D. Goz, P. Monaco, G. Murante & A. Curir, 2015, MNRAS, 447, 1774.
Galactic outflow and diffuse gas properties at z ≥ 1
using different baryonic feedback models,
P. Barai, P. Monaco, G. Murante, A. Ragagnin & M. Viel, 2015, MNRAS, 447, 266.