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Recent discoveries of carbon-enhanced metal-poor stars like SMSSJ031300.36-670839.3 provide increasing observational insights into theformation conditions of the first second-generation stars in the Universe,reflecting the chemical conditions after the first supernova explosion. Here,we present the first cosmological simulations with a detailed chemical networkincluding primordial species as well as C, C$^+$, O, O$^+$, Si, Si$^+$, andSi$^{2+}$ following the formation of carbon-enhanced metal poor stars. Thepresence of background UV flux delays the collapse from $z=21$ to $z=15$ andcool the gas down to the CMB temperature for a metallicity ofZ/Z$_\odot$=10$^{-3}$. This can potentially lead to the formation of lower massstars. Overall, we find that the metals have a stronger effect on the collapsethan the radiation, yielding a comparable thermal structure for largevariations in the radiative background. We further find that radiativebackgrounds are not able to delay the collapse for Z/Z$_\odot$=10$^{-2}$ or acarbon abundance as in SMSS J031300.36-670839.3.

Formation of carbon-enhanced metal-poor stars in the presence of far ultraviolet radiation