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

Stellar feedback, star formation and gravitational interactions are majorcontrolling forces in the evolution of Giant Molecular Clouds (GMCs). Toexplore their relative roles, we examine the properties and evolution of GMCsforming in an isolated galactic disk simulation that includes both localisedthermal feedback and photoelectric heating. The results are compared with thethree previous simulations in this series which consists of a model with nostar formation, star formation but no form of feedback and star formation withphotoelectric heating in a set with steadily increasing physical effects. Wefind that the addition of localised thermal feedback greatly suppresses starformation but does not destroy the surrounding GMC, giving cloud propertiesclosely resembling the run in which no stellar physics is included. Theoutflows from the feedback reduce the mass of the cloud but do not destroy it,allowing the cloud to survive its stellar children. This suggests that weakthermal feedback such as the lower bound expected for supernova may play arelatively minor role in the galactic structure of quiescent Milky Way-typegalaxies, compared to gravitational interactions and disk shear.

Star Formation in Disk Galaxies. III. Does stellar feedback result in cloud death?