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

In spite of decades of theoretical efforts, the physical origin of thestellar initial mass function (IMF) is still debated. We aim at understandingthe influence of various physical processes such as radiative stellar feedback,magnetic field and non-ideal magneto-hydrodynamics on the IMF. We present aseries of numerical simulations of collapsing 1000 M$_\odot$ clumps taking intoaccount radiative feedback and magnetic field with spatial resolution down to 1AU. Both ideal and non-ideal MHD runs are performed and various radiativefeedback efficiencies are considered. We also develop analytical models that weconfront to the numerical results. The sum of the luminosities produced by thestars in the calculations is computed and it compares well with the bolometricluminosities reported in observations of massive star forming clumps. Thetemperatures, velocities and densities are also found to be in good agreementwith recent observations. The stellar mass spectrum inferred for thesimulations is, generally speaking, not strictly universal and in particularvaries with magnetic intensity. It is also influenced by the choice of theradiative feedback efficiency. In all simulations, a sharp drop in the stellardistribution is found at about $M_{min} \simeq$ 0.1 M$_\odot$, which is likelya consequence of the adiabatic behaviour induced by dust opacities at highdensities. As a consequence, when the combination of magnetic and thermalsupport is not too large, the mass distribution presents a peak located at0.3-0.5 M$_\odot$. When magnetic and thermal support are large, the massdistribution is better described by a plateau, i.e. $d N / d \log M \proptoM^{-\Gamma}$, $\Gamma \simeq 0$. Abridged

How magnetic field and stellar radiative feedback influences the collapse and the stellar mass spectrum of a massive star forming clump