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 Tools annual

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 monthly

Global: Zendy Plus monthly

Presents the access of premium content as premium feature

Premium Content

Global: Zendy Plus annual

Global: Zendy Free Plan

The pressure exerted by massive stars' radiation fields is an importantmechanism regulating their formation. Detailed simulation of massive starformation therefore requires an accurate treatment of radiation. However, allpublished simulations have either used a diffusion approximation of limitedvalidity; have only been able to simulate a single star fixed in space, therebysuppressing potentially-important instabilities; or did not provide adequateresolution at locations where instabilities may develop. To remedy this we havedeveloped a new, highly accurate radiation algorithm that properly treats theabsorption of the direct radiation field from stars and the re-emission andprocessing by interstellar dust. We use our new tool to performthree-dimensional radiation-hydrodynamic simulations of the collapse of massivepre-stellar cores with laminar and turbulent initial conditions and properlyresolve regions where we expect instabilities to grow. We find that mass ischanneled to the stellar system via gravitational and Rayleigh-Taylor (RT)instabilities, in agreement with previous results using stars capable ofmoving, but in disagreement with methods where the star is held fixed or withsimulations that do not adequately resolve the development of RT instabilities.For laminar initial conditions, proper treatment of the direct radiation fieldproduces later onset of instability, but does not suppress it entirely providedthe edges of radiation-dominated bubbles are adequately resolved. Instabilitiesarise immediately for turbulent pre-stellar cores because the initialturbulence seeds the instabilities. Our results suggest that RT features aresignificant and should be present around accreting massive stars throughouttheir formation.

An Unstable Truth: How Massive Stars get their Mass