Simulations of star-forming main-sequence galaxies in Milgromian gravity
The result's identifiers
Result code in IS VaVaI
<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F23%3A10476048" target="_blank" >RIV/00216208:11320/23:10476048 - isvavai.cz</a>
Result on the web
<a href="https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=fFSuJckeDg" target="_blank" >https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=fFSuJckeDg</a>
DOI - Digital Object Identifier
<a href="http://dx.doi.org/10.1093/mnras/stac3645" target="_blank" >10.1093/mnras/stac3645</a>
Alternative languages
Result language
angličtina
Original language name
Simulations of star-forming main-sequence galaxies in Milgromian gravity
Original language description
We conduct hydrodynamical MOND simulations of isolated disc galaxies over the stellar mass range M-star/M-circle dot = 10(7)-10(11) using the adaptive mesh refinement code PHANTOM OF RAMSES (POR), an adaptation of the ramses code with a Milgromian gravity solver. The scale lengths and gas fractions are based on observed galaxies, and the simulations are run for 5 Gyr. The main aim is to see whether the existing sub-grid physics prescriptions for star formation and stellar feedback reproduce the observed main sequence and reasonably match the Kennicutt-Schmidt relation, which captures how the local and global star formation rates relate to other properties. Star formation in the models starts soon after initialization and continues as the models evolve. The initialized galaxies indeed evolve to a state which is on the observed main sequence and the Kennicutt-Schmidt relation. The available formulation of sub-grid physics is therefore adequate and leads to galaxies that largely behave like observed galaxies, grow in radius, and have flat rotation curves - provided we use Milgromian gravitation. Furthermore, the strength of the bars tends to be inversely correlated with the stellar mass of the galaxy, whereas the bar length strongly correlates with the stellar mass. Irrespective of the mass, the bar pattern speed stays constant with time, indicating that dynamical friction does not affect the bar dynamics. The models demonstrate Renzo's rule and form structures at large radii, much as in real galaxies. In this framework, baryonic physics is thus sufficiently understood to not pose major uncertainties in our modelling of global galaxy properties.
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
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Continuities
I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace
Others
Publication year
2023
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
0035-8711
e-ISSN
1365-2966
Volume of the periodical
519
Issue of the periodical within the volume
4
Country of publishing house
GB - UNITED KINGDOM
Number of pages
21
Pages from-to
5128-5148
UT code for WoS article
000927910000004
EID of the result in the Scopus database
2-s2.0-85160199547