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

Regulating the available gas mass inside galaxies proceeds through a delicatebalance between inflows and outflows, but also through the internal depletionof gas due to star formation. At the same time, stellar feedback is theinternal engine that powers the strong outflows. Since star formation andstellar feedback are both small scale phenomena, we need a realistic andpredictive subgrid model for both. We describe the implementation of supernovamomentum feedback and star formation based on the turbulence of the gas in theRAMSES code. For star formation, we adopt the so-called multi-freefall model.The resulting star formation efficiencies can be significantly smaller orbigger than the traditionally chosen value of $1\%$. We apply these newnumerical models to a prototype cosmological simulation of a massive halo thatfeatures a major merger which results in the formation of an early-type galaxywithout using AGN feedback. We find that the feedback model provides the firstorder mechanism for regulating the stellar and baryonic content in oursimulated galaxy. At high redshift, the merger event pushes gas to largedensities and large turbulent velocity dispersions, such that efficiencies comeclose to $10\%$, resulting in large SFR. We find small molecular gas depletiontime during the starburst, in perfect agreement with observations. Furthermore,at late times, the galaxy becomes quiescent with efficiencies significantlysmaller than $1\%$, resulting in small SFR and long molecular gas depletiontime.

Forming early-type galaxies without AGN feedback: a combination of merger-driven outflows and inefficient star formation