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 Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

An analysis of negative radiative feedback from resident stars in minihalosis performed. It is found that the most effective mechanism to suppress starformation is provided by infrared photons from resident stars viaphoto-detachment of ${\rm H^-}$. It is shown that a stringent upper bound on(total stellar mass, metallicity) of ($\sim 1000{\rm M_\odot}$, $-3.3\pm 0.2$)in any newly minted atomic cooling halo can be placed, with the actual valuespossibly significantly lower. This has both important physical ramifications onformation of stars and supermassive black seeds in atomic cooling halos at highredshift, pertaining to processes of low temperature metal cooling, dustformation and fragmentation, and direct consequences on the faint end galaxyluminosity function at high redshift and cosmological reionization. Theluminosity function of galaxies at the epoch of reionization may besubstantially affected due to the combined effect of a diminished role ofminihalos and an enhanced contribution from Pop III stars in atomic coolinghalos. Upcoming results on reionization optical depth from PlanckHigh-Frequency Instrument data may provide a significant constraint on and aunique probe of this star formation physical process in minihalos. As anumerical example, in the absence of significant contributions from minihaloswith virial masses below $1.5\times 10^{8}{\rm M_\odot}$ the reionizationoptical depth is expected to be no greater than $0.065$, whereas allowing forminihalos of masses as low as ($10^7{\rm M_\odot}$, $10^{6.5}{\rm M_\odot}$) toform stars unconstrained by this self-regulation physical process, thereionization optical depth is expected to exceed $(0.075,0.085)$, respectively.

Upper Limit on Star Formation and Metal Enrichment in Minihalos