[PDF] Top 20 Dynamical Masses of Young Star Clusters: Constraints on the Stellar IMF and Star-Formation Efficiency

... of young clusters with N-body simulations of clusters including the effects of rapid gas loss, we argue that young clusters are not in Virial ...determine dynamical ... See full document

... turbulent, star-forming giant molec- ular clouds (GMCs) with stellar feedback is described, extending previous work by simulating 10 different random realizations for each point in the parameter space of ... See full document

... other young clusters down to a mass of ∼ 1 M # and that the mass function could be fitted with a slope of # = − ...of stellar masses with a Kroupa et al. (2001) IMF, we identify the ... See full document

... ) stellar population in a sample of massive young clusters, we have targeted the ∼ 2 Myr old cluster NGC ...eld. Masses and extinctions of the candidate members are then calculated with the ... See full document

... neutron star theory prior to the discovery was concerned about constructing a model EOS of dense stellar ...neutron star and calculated the EOS of neutron star cores composed of free neutrons, ... See full document

... When ZAMS mass di ff erence is bigger than 4%, the di ff erence in their lifetime is bigger than 10%. Progenitors of NSs spend 90% of their lifetime in main sequence. So, in this case, when the primary NS is formed, the ... See full document

... reference star must be within 2^ in each co-ordinate but not so close- as to contribute appreciably to ; the measured li^t; a star with 1KY<C13 is most suitable# These requirements imposed a severe ... See full document

... According to WUM, all stable particles are created in the 3-sphere World due to the surface energy of the 4-ball Nucleus of the World provided by the 4-dimensional Universe. The World consists of the Medium (protons, ... See full document

... simulations of galaxies with up to subparsec resolution in which stars form when n H, * > 1000 cm - 3 and including momentum feedback representing stellar winds, radiation pressure and supernovae, and an ... See full document

... merger-induced star formation will take place in the central regions of the galaxy on subkpc scales ...give young YSP ages in Mrk 231 (Canalizo & Stockton 2001), J0025 − 10 (Bessiere et ... See full document

... The comparison of star cluster TO and White Dwarf (WD) ages has very recently confirmed the efficiency of a new physical process at work in the interior of WDs. HST observations of the well populated WD ... See full document

... in stellar mass ...considering star-forming galax- ies only, with log 10 (sSF R) > ...selecting star-forming galaxies, we find no difference be- tween the median SFRs in low and high density ... See full document

... The stellar wind from the central star with passive nebula is different from the wind of active accretion ...a star with a passive disk is almost equal to or greater than that of wind from solar-like ... See full document

... continuous star formation decline with τ> 5 × 10 8 yr, and the dashed lines are for star formation bursts with τ< 5 × 10 8 ... See full document

... Now LEGA-C is obtaining spectra of similar quality for ∼ 3200 K-band selected galaxies in the redshift range 0.6 < z < 1.0, at a lookback time of 6 – 8 Gyr. LEGA-C is a 4 year, 128-night Public Spectroscopic ... See full document

... of stellar age, stellar mass, SFR, and E(B-V) were made to study galaxy’s substructure on kiloparsec ...of star formation, and location of mass ...concentrated star formation and ... See full document

... low-metallicity star- forming galaxies in the early ...intensely star-forming sys- tems, and are thought to be comparable to the population whose ultraviolet flux caused the reionization of the Universe ... See full document

... galaxy formation and evolution is modeled by the Λ CDM, which stands for Cold Dark Mat- ter with dark energy field identified by ‘Λ’, the cosmological ...galaxy clusters (see Bartelmann &Schneider ... See full document

... in star formation history, they are indicative of the differences in behaviour between different ...total stellar mass would be measured using an SED fitting technique, and the star ... See full document

... four clusters shown in Figures 2.9–2.13 sample three star formation regions within the Antennae: the western loop (Clusters 79 and 104), the northeast (Cluster 82), and the overlap region ... See full document