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 introduce the {\em Phoenix Simulations}, a suite of highly resolvedcosmological simulations featuring hydrodynamics, primordial gas chemistry,Population III and II star formation and feedback, UV radiative transfer, andsaved outputs with $\Delta t$=200 kyr. The suite samples 73,523 distinctprimordial star formation events within \npiii distinct regions, forming \ngiisecond-generation enriched star clusters by $z \geq 12$ within a cumulative156.25 Mpc$^3$ volume. The regions that lead to enriched star formation containup to $167$ primordial stars, with 78.7 \% of regions having experiencedmultiple types of primordial supernovae. The extent of a primordial region,measured by its metal-rich surrounding cloud, is highly variable: the averageregion has radius $\sim 3$ kpc, with 95 \% confidence limit on the distributionof measured radii is $\sim 5-7$ kpc. For continuing star formation, we findthat the metallicity distribution of second generation stars is similar to thatof subsequent Population II star formation, with both distributions spanninghyper metal-deficient ([Z/H]$\sim-7$) to super-solar ([Z/H]$\sim0.8$). We findthat the metallicity of second generation stars has no strong dependence on theconfiguration of progenitor supernovae, with the mean metallicity ofsecond-generation stars having $-1.73 < $[Z/H]$<-2.15$. Finally, we create aninterpretable regression model to predict the radius of metal-rich influence of\piii star systems within the first 7-18 Myr after the first light. The modelpredicts the radius with $R_2 \gtrsim 0.4$ and mean squared error $\leq 0.06$.The probability distribution function of predicted radii compares well to thatof observed radii with Jensen-Shannon distance $\lesssim 0.2$ for all modelledtimes.

Connecting Primordial Star Forming Regions and Second Generation Star Formation in the Phoenix Simulations