The modelling of feedback in star formation simulations
Section snippets
Introduction and scope of this review
The formation of stars is arguably the most important process in astrophysics, impacting virtually every theoretical and observational subfield. Despite its prominence and decades of intensive study, there is still much about star formation that is not understood. One reason for this slow progress is the fact that the conversion of gas to stars is a non-linear process. There are a variety of reasons for this, such as the non-linearity of the self-gravitational forces which lead to the collapse
Brief introduction to stellar feedback physics
Stellar feedback involves the insertion of matter, momentum and energy from stars into the surrounding fluid, from which the stars may also still be accreting gas. In terms of material, momentum and energy emitted per star, massive OB-type stars far outweigh their lower-mass brethren in importance. In clouds where there are no O-stars (either because the cloud mass is too small to support massive star formation, or because there has not been time for O-stars to form), feedback from low- and
Brief introduction to astrophysical fluid dynamics codes
Star formation takes place in the interstellar medium (ISM), the thin and usually hot gas which occupies much of the volume of most galaxies. The mean free paths of ions, atoms and molecules in the ISM tend to be small compared with the sizes of the structures which they belong to. It is therefore reasonable to approximate the ISM as a smoothly-varying fluid. However, in order to model the behaviour of a fluid on a computer, it is necessary to discretise it in some way into individual fluid
Feedback algorithms
This section briefly surveys some of the algorithms used to model stellar feedback mechanisms. The focus is on the algorithms themselves and the assumptions that underlie them. The results gained from using them will be discussed in a later section.
What we have learned from including feedback in simulations
The previous section concentrated on technical descriptions of algorithms and is intended to be mainly of use to researchers who are considering writing their own feedback prescription and wish to get an overview of how it has been done before. This section is aimed at a different readership and will concentrate on the science results of simulations run using the algorithms and codes described. There will inevitably be a small amount of repetition and overlap between these two sections, so some
Summary and outlook
The last decade has seen the development of a tremendous variety of sophisticated algorithms to model the various kinds of stellar feedback, and a corresponding wealth of simulations employing these algorithms to answer a wide variety of questions over a huge range of scales. We have learned an enormous amount from these simulations.
Feedback regulates or helps to regulate the rate at which gas is converted to stars at every stage of the star formation process. The background cosmic ionising
Acknowledgements
The author is grateful for the support of the DFG cluster of excellence ‘Origin and Structure of the Universe’. In writing this review, he has made extensive use of the nasa/sao ads literature search engine and of the papers software package (http://www.papersapp.com), without either of which the process would have been much longer and more tedious. The author is also grateful to David Hubber for useful discussions of numerical methods, and to the referee, Ant Whitworth, for a
References (250)
- et al.
Radiation feedback in ULIRGs: Are photons movers and shakers?
Astrophys. J.
(2014) - et al.
Multi-dimensional cosmological radiative transfer with a variable eddington tensor formalism
NewA
(2001) - et al.
Simulations of galaxy formation in a Λ cold dark matter universe. I. Dynamical and photometric properties of a simulated disk galaxy
Astrophys. J.
(2003) - et al.
Adaptive ray tracing for radiative transfer around point sources
Mon. Not. R. Astron. Soc.
(2002) - et al.
On the interplay between star formation and feedback in galaxy formation simulations
Astrophys. J.
(2015) - et al.
Toward a complete accounting of energy and momentum from stellar feedback in galaxy formation simulations
Astrophys. J.
(2013) - et al.
Fundamental differences between SPH and grid methods
Mon. Not. R. Astron. Soc.
(2007) - et al.
The formation of disc galaxies in a ΛCDM universe
Mon. Not. R. Astron. Soc.
(2011) - et al.
SPHRAY: a smoothed particle hydrodynamics ray tracer for radiative transfer
Mon. Not. R. Astron. Soc.
(2008) What produces the diffuse X-ray emission from the orion nebula? I. Simple spherical models
Mon. Not. R. Astron. Soc.
(2012)
Radiation-magnetohydrodynamic simulations of H II regions and their associated PDRs in turbulent molecular clouds
Mon. Not. R. Astron. Soc.
Hydrodynamics of cometary compact H II regions
Astrophys. J. Suppl.
Towards a more realistic population of bright spiral galaxies in cosmological simulations
Mon. Not. R. Astron. Soc.
Shapes and shaping of planetary nebulae
Ann. Rev. Astron. Astrophys.
Can protostellar jets drive supersonic turbulence in molecular clouds?
Astrophys. J.
The importance of radiative feedback for the stellar initial mass function
Mon. Not. R. Astron. Soc.
The statistical properties of stars and their dependence on metallicity: the effects of opacity
Mon. Not. R. Astron. Soc.
Modelling accretion in protobinary systems
Mon. Not. R. Astron. Soc.
Combining radiative transfer and diffuse interstellar medium physics to model star formation
Mon. Not. R. Astron. Soc.
The photoevaporation of interstellar clouds. I – radiation-driven implosion
Astrophys. J.
Smoothed particle hydrodynamics simulations of expanding H II regions. I. Numerical method and applications
Astron. Astrophys.
Radiation-driven implosion and triggered star formation
Astrophys. J.
Turbulence in giant molecular clouds: the effect of photoionization feedback
Mon. Not. R. Astron. Soc.
Shocks, cooling and the origin of star formation rates in spiral galaxies
Mon. Not. R. Astron. Soc.
MaGICC discs: matching observed galaxy relationships over a wide stellar mass range
Mon. Not. R. Astron. Soc.
Relative effects of ionizing radiation and winds from O-type stars on the structure and dynamics of H II regions
Publ. Astron. Sco. Pac.
Outflow-driven turbulence in molecular clouds
Astrophys. J.
Interstellar bubbles
ApJL
Radiative feedback and the low efficiency of galaxy formation in low-mass haloes at high redshift
Mon. Not. R. Astron. Soc.
On column density thresholds and the star formation rate
Mon. Not. R. Astron. Soc.
TreeCol: a novel approach to estimating column densities in astrophysical simulations
Mon. Not. R. Astron. Soc.
How long does it take to form a molecular cloud?
Mon. Not. R. Astron. Soc.
The formation and fragmentation of disks around primordial protostars
Science
Molecular cloud evolution - V. Cloud destruction by stellar feedback
Mon. Not. R. Astron. Soc.
The EAGLE simulations of galaxy formation: calibration of subgrid physics and model variations
Mon. Not. R. Astron. Soc.
Radiation-hydrodynamic simulations of massive star formation with protostellar outflows
Astrophys. J.
Ionizing feedback from massive stars in massive clusters: fake bubbles and untriggered star formation
Mon. Not. R. Astron. Soc.
The effect of stellar winds on the formation of a protocluster
Mon. Not. R. Astron. Soc.
Ionization-induced star formation – III. Effects of external triggering on the initial mass function in clusters
Mon. Not. R. Astron. Soc.
Photoionizing feedback in star cluster formation
Mon. Not. R. Astron. Soc.
Ionization-induced star formation – I. The collect-and-collapse model
Mon. Not. R. Astron. Soc.
Ionization-induced star formation – II. External irradiation of a turbulent molecular cloud
Mon. Not. R. Astron. Soc.
Ionization-induced star formation – IV. Triggering in bound clusters
Mon. Not. R. Astron. Soc.
Ionizing feedback from massive stars in massive clusters – II. Disruption of bound clusters by photoionization
Mon. Not. R. Astron. Soc.
Ionization-induced star formation – V. Triggering in partially unbound clusters
Mon. Not. R. Astron. Soc.
Ionizing feedback from massive stars in massive clusters – III. Disruption of partially unbound clouds
Mon. Not. R. Astron. Soc.
A new algorithm for modelling photoionizing radiation in smoothed particle hydrodynamics
Mon. Not. R. Astron. Soc.
The dangers of being trigger-happy
Mon. Not. R. Astron. Soc.
Massive stars in massive clusters – IV. Disruption of clouds by momentum-driven winds
Mon. Not. R. Astron. Soc.
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