The kinematics of star clusters undergoing gas expulsion in Newtonian and Milgroniian dynamics
Identifikátory výsledku
Kód výsledku v IS VaVaI
<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F19%3A10406400" target="_blank" >RIV/00216208:11320/19:10406400 - isvavai.cz</a>
Výsledek na webu
<a href="https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=3196Lw4prX" target="_blank" >https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=3196Lw4prX</a>
DOI - Digital Object Identifier
<a href="http://dx.doi.org/10.1093/mnras/stz1519" target="_blank" >10.1093/mnras/stz1519</a>
Alternativní jazyky
Jazyk výsledku
angličtina
Název v původním jazyce
The kinematics of star clusters undergoing gas expulsion in Newtonian and Milgroniian dynamics
Popis výsledku v původním jazyce
We study the kinematics of stars in clusters undergoing gas expulsion in standard Newtonian dynamics and also in Milgromian dynamics (MOND). Gas expulsion can explain the observed line-of-sight (LoS) velocity dispersion profile of NGC 2419 in Newtonian dynamics. For a given star formation efficiency (SEE), the shapes of the velocity dispersion profiles, which are normalized by the velocity dispersion at the projected half-mass radius, are almost indistinguishable for different SEE models in Newtonian dynamics. The velocity dispersion of a star cluster in the outer halo of a galaxy can indeed have a strong radial anisotropy in Newtonian dynamics after gas expulsion. MOND displays several different properties from Newtonian dynamics. In particular, the slope of the central velocity dispersion profile is less steep in MOND for the same SFE. Moreover, for a given SFE, more massive embedded cluster models result in more rapidly declining central velocity dispersion profiles for the final star clusters, while less massive embedded cluster models lead to flatter velocity dispersion profiles for the final products. The onset of the radial-orbit instability in post-gas-expulsion MOND models is discussed. SFEs as low as a few per cent, typical of molecular clouds, lead to surviving ultradiffuse objects. Gas expulsion alone is unlikely the physical mechanism for the observed velocity dispersion profile of NGC 2419 in MOND.
Název v anglickém jazyce
The kinematics of star clusters undergoing gas expulsion in Newtonian and Milgroniian dynamics
Popis výsledku anglicky
We study the kinematics of stars in clusters undergoing gas expulsion in standard Newtonian dynamics and also in Milgromian dynamics (MOND). Gas expulsion can explain the observed line-of-sight (LoS) velocity dispersion profile of NGC 2419 in Newtonian dynamics. For a given star formation efficiency (SEE), the shapes of the velocity dispersion profiles, which are normalized by the velocity dispersion at the projected half-mass radius, are almost indistinguishable for different SEE models in Newtonian dynamics. The velocity dispersion of a star cluster in the outer halo of a galaxy can indeed have a strong radial anisotropy in Newtonian dynamics after gas expulsion. MOND displays several different properties from Newtonian dynamics. In particular, the slope of the central velocity dispersion profile is less steep in MOND for the same SFE. Moreover, for a given SFE, more massive embedded cluster models result in more rapidly declining central velocity dispersion profiles for the final star clusters, while less massive embedded cluster models lead to flatter velocity dispersion profiles for the final products. The onset of the radial-orbit instability in post-gas-expulsion MOND models is discussed. SFEs as low as a few per cent, typical of molecular clouds, lead to surviving ultradiffuse objects. Gas expulsion alone is unlikely the physical mechanism for the observed velocity dispersion profile of NGC 2419 in MOND.
Klasifikace
Druh
J<sub>imp</sub> - Článek v periodiku v databázi Web of Science
CEP obor
—
OECD FORD obor
10308 - Astronomy (including astrophysics,space science)
Návaznosti výsledku
Projekt
—
Návaznosti
I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace
Ostatní
Rok uplatnění
2019
Kód důvěrnosti údajů
S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů
Údaje specifické pro druh výsledku
Název periodika
Monthly Notices of the Royal Astronomical Society
ISSN
0035-8711
e-ISSN
—
Svazek periodika
487
Číslo periodika v rámci svazku
3
Stát vydavatele periodika
GB - Spojené království Velké Británie a Severního Irska
Počet stran výsledku
13
Strana od-do
4012-4024
Kód UT WoS článku
000478053200077
EID výsledku v databázi Scopus
2-s2.0-85072288824