Nonuniversal star formation efficiency in turbulent ISM
Abstract
Here, we present a study of a star formation prescription in which star formation efficiency depends on local gas density and turbulent velocity dispersion, as suggested by direct simulations of SF in turbulent giant molecular clouds (GMCs). We test the model using a simulation of an isolated Milky Way-sized galaxy with a self-consistent treatment of turbulence on unresolved scales. We show that this prescription predicts a wide variation of local star formation efficiency per free-fall time, $$\epsilon_{\rm ff} \sim 0.1 - 10\%$$, and gas depletion time, $$t_{\rm dep} \sim 0.1 - 10$$ Gyr. In addition, it predicts an effective density threshold for star formation due to suppression of $$\epsilon_{\rm ff}$$ in warm diffuse gas stabilized by thermal pressure. We show that the model predicts star formation rates in agreement with observations from the scales of individual star-forming regions to the kiloparsec scales. This agreement is non-trivial, as the model was not tuned in any way and the predicted star formation rates on all scales are determined by the distribution of the GMC-scale densities and turbulent velocities $$\sigma$$ in the cold gas within the galaxy, which is shaped by galactic dynamics. The broad agreement of the star formation prescription calibrated in the GMC-scale simulations with observations, both gives credence to such simulations and promises to put star formation modeling in galaxy formation simulations on a much firmer theoretical footing.
- Authors:
-
- The Univ. of Chicago, Chicago, IL (United States)
- The Univ. of Chicago, Chicago, IL (United States); Fermi National Accelerator Lab. (FNAL), Batavia, IL (United States)
- Publication Date:
- Research Org.:
- Fermi National Accelerator Laboratory (FNAL), Batavia, IL (United States)
- Sponsoring Org.:
- USDOE Office of Science (SC), High Energy Physics (HEP)
- OSTI Identifier:
- 1333137
- Report Number(s):
- arXiv:1512.03101; FERMILAB-PUB-16-503-A
Journal ID: ISSN 1538-4357; 1495139
- Grant/Contract Number:
- AC02-07CH11359
- Resource Type:
- Accepted Manuscript
- Journal Name:
- The Astrophysical Journal (Online)
- Additional Journal Information:
- Journal Name: The Astrophysical Journal (Online); Journal Volume: 826; Journal Issue: 2; Journal ID: ISSN 1538-4357
- Publisher:
- Institute of Physics (IOP)
- Country of Publication:
- United States
- Language:
- English
- Subject:
- 79 ASTRONOMY AND ASTROPHYSICS; galaxies: ISM; numerical; stars: formation; turbulence
Citation Formats
Semenov, Vadim A., Kravtsov, Andrey V., and Gnedin, Nickolay Y. Nonuniversal star formation efficiency in turbulent ISM. United States: N. p., 2016.
Web. doi:10.3847/0004-637X/826/2/200.
Semenov, Vadim A., Kravtsov, Andrey V., & Gnedin, Nickolay Y. Nonuniversal star formation efficiency in turbulent ISM. United States. https://doi.org/10.3847/0004-637X/826/2/200
Semenov, Vadim A., Kravtsov, Andrey V., and Gnedin, Nickolay Y. Fri .
"Nonuniversal star formation efficiency in turbulent ISM". United States. https://doi.org/10.3847/0004-637X/826/2/200. https://www.osti.gov/servlets/purl/1333137.
@article{osti_1333137,
title = {Nonuniversal star formation efficiency in turbulent ISM},
author = {Semenov, Vadim A. and Kravtsov, Andrey V. and Gnedin, Nickolay Y.},
abstractNote = {Here, we present a study of a star formation prescription in which star formation efficiency depends on local gas density and turbulent velocity dispersion, as suggested by direct simulations of SF in turbulent giant molecular clouds (GMCs). We test the model using a simulation of an isolated Milky Way-sized galaxy with a self-consistent treatment of turbulence on unresolved scales. We show that this prescription predicts a wide variation of local star formation efficiency per free-fall time, $\epsilon_{\rm ff} \sim 0.1 - 10\%$, and gas depletion time, $t_{\rm dep} \sim 0.1 - 10$ Gyr. In addition, it predicts an effective density threshold for star formation due to suppression of $\epsilon_{\rm ff}$ in warm diffuse gas stabilized by thermal pressure. We show that the model predicts star formation rates in agreement with observations from the scales of individual star-forming regions to the kiloparsec scales. This agreement is non-trivial, as the model was not tuned in any way and the predicted star formation rates on all scales are determined by the distribution of the GMC-scale densities and turbulent velocities $\sigma$ in the cold gas within the galaxy, which is shaped by galactic dynamics. The broad agreement of the star formation prescription calibrated in the GMC-scale simulations with observations, both gives credence to such simulations and promises to put star formation modeling in galaxy formation simulations on a much firmer theoretical footing.},
doi = {10.3847/0004-637X/826/2/200},
journal = {The Astrophysical Journal (Online)},
number = 2,
volume = 826,
place = {United States},
year = {Fri Jul 29 00:00:00 EDT 2016},
month = {Fri Jul 29 00:00:00 EDT 2016}
}
Web of Science
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Observational Evidence of Dynamic Star Formation Rate in Milky Way Giant Molecular Clouds
text, January 2016
- Lee, Eve J.; Miville-Deschenes, Marc-Antoine; Murray, Norman
- arXiv
What drives gravitational instability in nearby star-forming spirals? The impact of CO and HI velocity dispersions
text, January 2017
- Romeo, Alessandro B.; Mogotsi, Keoikantse Moses
- arXiv
Star Cluster Formation in Cosmological Simulations. II. Effects of Star Formation Efficiency and Stellar Feedback
text, January 2017
- Li, Hui; Gnedin, Oleg Y.; Gnedin, Nickolay Y.
- arXiv
On the Appearance of Thresholds in the Dynamical Model of Star Formation
text, January 2018
- Elmegreen, Bruce G.
- arXiv
Globular Cluster Formation and Evolution in the Context of Cosmological Galaxy Assembly: Open Questions
text, January 2018
- Forbes, Duncan A.; Bastian, Nate; Gieles, Mark
- arXiv
The Fate of Supernova-Heated Gas in Star-Forming Regions of the LMC: Lessons for Galaxy Formation?
text, January 2018
- Bustard, Chad; Pardy, Stephen A.; D'Onghia, Elena
- arXiv
An uncertainty principle for star formation - II. A new method for characterising the cloud-scale physics of star formation and feedback across cosmic history
text, January 2018
- Kruijssen, J. M. Diederik; Schruba, Andreas; Hygate, Alexander P. S.
- arXiv
The [CII]--SFR correlation in dwarf galaxies across cosmic time
text, January 2019
- Lupi, Alessandro; Bovino, Stefano
- arXiv
Fast and inefficient star formation due to short-lived molecular clouds and rapid feedback
text, January 2019
- Kruijssen, J. M. Diederik; Schruba, Andreas; Chevance, Mélanie
- arXiv
Forming early-type galaxies without AGN feedback: a combination of merger-driven outflows and inefficient star formation
text, January 2019
- Kretschmer, Michael; Teyssier, Romain
- arXiv