English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

We compute different sets of stellar evolutionary tracks in order to quantifythe energy, mass, and metals yielded by massive main-sequence andpost-main-sequence winds. Our aim is to investigate the impact of binarysystems and of a metallicity-dependent distribution of initial rotationalvelocities on the feedback by stellar winds. We find significant changescompared to the commonly used non-rotating, single-star scenario. The largestdifferences are noticeable at low metallicity, where the mechanical-energybudget is substantially increased. So as to establish the maximal (i.e.obtained by neglecting dissipation in the near circumstellar environment)influence of winds on the early stages of galaxy formation, we use our newfeedback estimates to simulate the formation and evolution of a sub-$L_*$galaxy at redshift 3 (hosted by a dark-matter halo with a mass of $1.8\times10^{11}$ M$_\odot$) and compare the outcome with simulations in which onlysupernova (SN) feedback is considered. Accounting for the continuous energyinjection by winds reduces the total stellar mass, the metal content, and theburstiness of the star-formation rate as well as of the outflowing gas mass.However, our numerical experiment suggests that the enhanced mechanicalfeedback from the winds of rotating and binary stars has a limited impact onthe most relevant galactic properties compared to the non-rotating single-starscenario. Eventually, we look at the relative abundance between the metalsentrained in winds and those ejected by SNe and find that it stays nearlyconstant within the simulated galaxy and its surrounding halo.

Mechanical feedback from stellar winds with an application to galaxy formation at high redshift