The SILCC project III. Regulation of star formation and outflows by stellar winds and supernovae
The result's identifiers
Result code in IS VaVaI
<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F17%3A00484760" target="_blank" >RIV/67985815:_____/17:00484760 - isvavai.cz</a>
Result on the web
<a href="https://doi.org/10.1093/mnras/stw3209" target="_blank" >https://doi.org/10.1093/mnras/stw3209</a>
DOI - Digital Object Identifier
<a href="http://dx.doi.org/10.1093/mnras/stw3209" target="_blank" >10.1093/mnras/stw3209</a>
Alternative languages
Result language
angličtina
Original language name
The SILCC project III. Regulation of star formation and outflows by stellar winds and supernovae
Original language description
We study the impact of stellar winds and supernovae on the multiphase interstellar medium using three-dimensional hydrodynamical simulations carried out with FLASH. The selected galactic disc region has a size of (500 pc)(2) x +/- 5 kpc and a gas surface density of 10M(circle dot) pc(-2). The simulations include an external stellar potential and gas self-gravity, radiative cooling and diffuse heating, sink particles representing star clusters, stellar winds from these clusters that combine the winds from individual massive stars by following their evolution tracks, and subsequent supernova explosions. Dust and gas (self-) shielding is followed to compute the chemical state of the gas with a chemical network. We find that stellar winds can regulate star (cluster) formation. Since the winds suppress the accretion of fresh gas soon after the cluster has formed, they lead to clusters that have lower average masses (10(2)-10(4.3)M(circle dot)) and form on shorter time-scales (10(-3)-10 Myr). In particular, we find an anticorrelation of cluster mass and accretion time-scale. Without winds, the star clusters easily grow to larger masses for similar to 5 Myr until the first supernova explodes. Overall, the most massive stars provide the most wind energy input, while objects beginning their evolution as B-type stars contribute most of the supernova energy input. A significant outflow from the disc (mass loading greater than or similar to 1 at 1 kpc) can be launched by thermal gas pressure if more than 50 per cent of the volume near the disc mid-plane can be heated to T > 3 x 10(5) K. Stellar winds alone cannot create a hot volume-filling phase. The models that are in best agreement with observed star formation rates drive either no outflows or weak outflows.
Czech name
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Czech description
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Classification
Type
J<sub>imp</sub> - Article in a specialist periodical, which is included in the Web of Science database
CEP classification
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OECD FORD branch
10308 - Astronomy (including astrophysics,space science)
Result continuities
Project
<a href="/en/project/GA15-06012S" target="_blank" >GA15-06012S: Multi-Generation Star Clusters</a><br>
Continuities
P - Projekt vyzkumu a vyvoje financovany z verejnych zdroju (s odkazem do CEP)
Others
Publication year
2017
Confidentiality
S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů
Data specific for result type
Name of the periodical
Monthly Notices of the Royal Astronomical Society
ISSN
1365-2966
e-ISSN
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Volume of the periodical
466
Issue of the periodical within the volume
2
Country of publishing house
GB - UNITED KINGDOM
Number of pages
22
Pages from-to
1903-1924
UT code for WoS article
000398284600044
EID of the result in the Scopus database
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