Αποτελέσματα Αναζήτησης
18 Απρ 2023 · We investigate the stability of nearby disc galaxies and galaxies at redshift (z) equal to 4.5. We explore the connection between the stability parameter (QRW), star formation rate (S FR), gas fraction (fGas), and the time scale for growth of gravitational instabil-ities ( ).
25 Ιουλ 2016 · Given the tight correlations between \(M_{\star}\) and SFR, and between SFR and \(\mbox{H}_{2}\)-mass, it is straightforward to model the evolution of \(f_{\mathrm{gas}}\) in main sequence galaxies where \(M_{\mathrm{gas}}/M_{\star} \equiv \mbox{const.} \times \mbox{SFR}(M_{\star})^{\beta_{\text{K-S}}}/M_{\star}\).
31 Μαρ 2020 · A Model for the Onset of Self-gravitation and Star Formation in Molecular Gas Governed by Galactic Forces. II. The Bottleneck to Collapse Set by Cloud–Environment Decoupling.
In this work we update the L-Galaxies semi-analytic model (SAM) to better follow the physical processes responsible for the growth of bulges via disc instabilities (leading to pseudo-bulges) and mergers (leading to classical bulges).
13 Ιουλ 2022 · Hydrodynamical simulations enable us to precisely reconstruct the SFH of galaxies and establish a link to the underlying physical processes. In this work, we present a model to describe individual galaxies’ SFHs from three simulations: TheThreeHundred, Illustris-1, and TNG100-1.
18 Απρ 2023 · In this work, we have studied the stability of the nearby galaxies, which are a part of the SPARC catalogue, using the two-component stability criterion proposed by Romeo & Wiegert . We find: The net stability in the galaxies are primarily driven by the stellar disc.
30 Μαρ 2019 · We investigate the structure of galaxies formed in a suite of high-resolution cosmological simulations. Consistent with observations of high-redshift galaxies, our simulated galaxies show irregular, prolate shapes, which are dominated by turbulent motions instead of rotation.
