Stellar ram pressure3/13/2023 Optical to far-infrared isochrones with improved TP-AGB models. Evolution of asymptotic giant branch stars. Globular cluster mass loss in the context of multiple populations. ![]() Origin of multiple stellar populations in globular clusters and their helium enrichment. Secondary star formation within massive star clusters: origin of multiple stellar populations in globular clusters. Formation and dynamical evolution of multiple stellar generations in globular clusters. ω Centauri: the population puzzle goes deeper. Multiple stellar populations in 47 Tucanae. A triple main sequence in the globular cluster NGC 2808. Lessons learned from the Milky Way globular clusters. Multiple populations in globular clusters. This process may eventually give rise to the ubiquitous multiple stellar populations in globular clusters. We show that such clusters could have accreted sufficient gas to form new stars if they had orbited in their host galaxies’ gaseous disks throughout the period between their initial formation and the more recent bursts of star formation. Here we report observations of three massive relatively young star clusters (1–2 billion years old) in the Magellanic Clouds that show clear evidence of burst-like star formation that occurred a few hundred million years after their initial formation era. For this to occur 8, the initial cluster masses need to be greater than a few million solar masses. Colliding stellar winds from late-stage, asymptotic-giant-branch stars 5, 6, 7 are often suggested to be triggers of second-generation star formation. However, massive, old ‘globular’ clusters-those with ages greater than ten billion years and masses several hundred thousand times that of the Sun-often harbour multiple stellar populations 1, 2, 3, 4, indicating that more than one star-forming event occurred during their lifetimes. Into the wake on very short timescales.Stars in clusters are thought to form in a single burst from a common progenitor cloud of molecular gas. Ram-pressure stripping can shift the location of star formation from the disc With surface densities locally comparable to values in the inner stellar disc. Young stars can be found throughout the stripped wake Continuously stars fall back to the old stellar disc, building upĪ bulge-like structure. In the wake of the galaxy out to distances of more than 350 kpc behind the Up to 95% of all newly formed stars can be found TheĮnhancement of the star formation depends more on the surrounding gas density The relative velocity was varied from 100 km/s to 1000 km/s inĭifferent surrounding gas densities in the range from $1\times10^$ĭyn/cm$^2$) in comparison to the same system evolving in isolation. All gas particles within the computational domain having the same Special emphasis was put on the gas within the disc and in the (GADGET-2) with radiative cooling and a recipe for star formation and stellarįeedback 12 different ram-pressure stripping scenarios for disc galaxies wereĬalculated. ![]() By applying a combined N-body/hydrodynamic description Observations in X-ray, H$\alpha$ and HI wavelength for different ram-pressure Ziegler Download PDF Abstract: We investigate the dependence of star formation and the distribution of theĬomponents of galaxies on the strength of ram pressure.
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