Galactic chemical evolution models are crucial ingredients to place first, broad constraints on the limits and the evolution of the Galactic Habitable Zone (GHZ), as well as for the conditions for life formation within our Galaxy. In fact, by comparing model predictions of element abundances with observations from different stellar populations and the interstellar medium (ISM), we can place...
Theoretical studies of galactic habitable zones (GHZs) have predominantly focused on the Local Neighbourhood, Milky Way, or the Local Group. However, with the establishment of the latest wave of cutting-edge observational instrumentation, GHZ indicators can now be observed in large numbers of other galaxies out to much further distances that ever before. This highlights the need for...
The Galactic habitable zone is defined as the region with a metallicity that is high enough to form planetary systems in which Earth-like planets could be born and might be capable of sustaining life. Life in this zone needs to survive the destructive effects of nearby supernova explosion events. Our aim is to find the Galactic habitable zone using chemical evolution models for the Milky Way...
The chemical evolution of the elements in the Milky Way is a key diagnostic to understand the enrichment history and the abundance distribution of metals necessary to form Earth-like planets in the Sun and in other stars in the solar neighborhood. The production of specific elemental ratios (and isotopes) can be used to constrain different uncertainties affecting galactic chemical evolution...
The formation of environments on the galactic scale that are suitable for the presence of life requires a sufficient amount of metals in the interstellar medium to trigger planet formation, but at the same time low rates of potentially life-harmful events such as Supernovae and Gamma-ray bursts.
Although evolved and massive galaxies, like our Milky Way, are expected to form stars with...
