![]() ![]() Today the origin of the heaviest elements is still matter of debate. These compact objects may also merge, leading to a new ejection of material. Small stars like our Sun end their life as planetary nebulae, while more massive stars end their evolution with violent explosions like supernovae or hypernovae, leaving behind either a neutron star or a black hole. Gas clouds form and collapse to stars, experiencing different evolutionary stages according to their properties like mass and metal content. Stars provide a fundamental contribution to the cosmic life cycle. Inhomogeneous galactic chemical evolution of r-process elements ![]() The main input parameters for this study were: a) The Neutron Star Merger (NSM) coalescence time scale, the probability of NSMs, and for the sub-class of â€magneto-rotationally driven Supernovae†(â€Jet-SNeâ€), their occurence rate in comparison to â€standard†Supernovae (SNe). For this work, we used the inhomogeneous GCE model â€ICEâ€, which allows to keep track of the galactic abundances of elements produced by different astrophysical sites. ![]() We report the results of a galactic chemical evolution (GCE) study for r-process- and alpha elements. Inhomogeneous chemical evolution of r-process elements ![]()
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