Advanced

Toward a complete accounting of energy and momentum from stellar feedback in galaxy formation simulations

Agertz, Oscar LU ; Kravtsov, Andrey V.; Leitner, Samuel N. and Gnedin, Nickolay Y. (2013) In Astrophysical Journal 770(1).
Abstract

We investigate the momentum and energy budget of stellar feedback during different stages of stellar evolution, and study its impact on the interstellar medium (ISM) using simulations of local star-forming regions and galactic disks at the resolution affordable in modern cosmological zoom-in simulations. In particular, we present a novel subgrid model for the momentum injection due to radiation pressure and stellar winds from massive stars during early, pre-supernova (pre-SN) evolutionary stages of young star clusters. Early injection of momentum acts to clear out dense gas in star-forming regions, hence limiting star formation. The reduced gas density mitigates radiative losses of thermal feedback energy from subsequent SN explosions.... (More)

We investigate the momentum and energy budget of stellar feedback during different stages of stellar evolution, and study its impact on the interstellar medium (ISM) using simulations of local star-forming regions and galactic disks at the resolution affordable in modern cosmological zoom-in simulations. In particular, we present a novel subgrid model for the momentum injection due to radiation pressure and stellar winds from massive stars during early, pre-supernova (pre-SN) evolutionary stages of young star clusters. Early injection of momentum acts to clear out dense gas in star-forming regions, hence limiting star formation. The reduced gas density mitigates radiative losses of thermal feedback energy from subsequent SN explosions. The detailed impact of stellar feedback depends sensitively on the implementation and choice of parameters. Somewhat encouragingly, we find that implementations in which feedback is efficient lead to approximate self-regulation of the global star formation efficiency. We compare simulation results using our feedback implementation to other phenomenological feedback methods, where thermal feedback energy is allowed to dissipate over timescales longer than the formal gas cooling time. We find that simulations with maximal momentum injection suppress star formation to a similar degree as is found in simulations adopting adiabatic thermal feedback. However, different feedback schemes are found to produce significant differences in the density and thermodynamic structure of the ISM, and are hence expected to have a qualitatively different impact on galaxy evolution. © 2013. The American Astronomical Society. All rights reserved..

(Less)
Please use this url to cite or link to this publication:
author
publishing date
type
Contribution to journal
publication status
published
subject
keywords
galaxies: evolution, galaxies: ISM, ISM: structure, methods: numerical, stars: formation
in
Astrophysical Journal
volume
770
issue
1
publisher
University of Chicago Press
external identifiers
  • scopus:84878293031
ISSN
0004-637X
DOI
10.1088/0004-637X/770/1/25
language
English
LU publication?
no
id
fecb5c00-aaaa-43fa-a49e-e4e7538e46bf
date added to LUP
2016-08-16 22:58:29
date last changed
2017-10-01 05:22:18
@article{fecb5c00-aaaa-43fa-a49e-e4e7538e46bf,
  abstract     = {<p>We investigate the momentum and energy budget of stellar feedback during different stages of stellar evolution, and study its impact on the interstellar medium (ISM) using simulations of local star-forming regions and galactic disks at the resolution affordable in modern cosmological zoom-in simulations. In particular, we present a novel subgrid model for the momentum injection due to radiation pressure and stellar winds from massive stars during early, pre-supernova (pre-SN) evolutionary stages of young star clusters. Early injection of momentum acts to clear out dense gas in star-forming regions, hence limiting star formation. The reduced gas density mitigates radiative losses of thermal feedback energy from subsequent SN explosions. The detailed impact of stellar feedback depends sensitively on the implementation and choice of parameters. Somewhat encouragingly, we find that implementations in which feedback is efficient lead to approximate self-regulation of the global star formation efficiency. We compare simulation results using our feedback implementation to other phenomenological feedback methods, where thermal feedback energy is allowed to dissipate over timescales longer than the formal gas cooling time. We find that simulations with maximal momentum injection suppress star formation to a similar degree as is found in simulations adopting adiabatic thermal feedback. However, different feedback schemes are found to produce significant differences in the density and thermodynamic structure of the ISM, and are hence expected to have a qualitatively different impact on galaxy evolution. © 2013. The American Astronomical Society. All rights reserved..</p>},
  articleno    = {25},
  author       = {Agertz, Oscar and Kravtsov, Andrey V. and Leitner, Samuel N. and Gnedin, Nickolay Y.},
  issn         = {0004-637X},
  keyword      = {galaxies: evolution,galaxies: ISM,ISM: structure,methods: numerical,stars: formation},
  language     = {eng},
  month        = {06},
  number       = {1},
  publisher    = {University of Chicago Press},
  series       = {Astrophysical Journal},
  title        = {Toward a complete accounting of energy and momentum from stellar feedback in galaxy formation simulations},
  url          = {http://dx.doi.org/10.1088/0004-637X/770/1/25},
  volume       = {770},
  year         = {2013},
}