Simulations of star-forming main-sequence galaxies in Milgromian gravity

Kód výsledku v 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>

Výsledek na webu

<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>

Jazyk výsledku

angličtina

Název v původním jazyce

Simulations of star-forming main-sequence galaxies in Milgromian gravity

Popis výsledku v původním jazyce

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&apos;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.

Název v anglickém jazyce

Simulations of star-forming main-sequence galaxies in Milgromian gravity

Popis výsledku anglicky

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&apos;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.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

—

Návaznosti

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Rok uplatnění

2023

Kód důvěrnosti údajů

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Název periodika

Monthly Notices of the Royal Astronomical Society

ISSN

0035-8711

e-ISSN

1365-2966

Svazek periodika

519

Číslo periodika v rámci svazku

4

Stát vydavatele periodika

GB - Spojené království Velké Británie a Severního Irska

Počet stran výsledku

21

Strana od-do

5128-5148

Kód UT WoS článku

000927910000004

EID výsledku v databázi Scopus

2-s2.0-85160199547