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We explore the possibility of planet formation in the carbon-richprotoplanetary disks of carbon-enhanced metal-poor (CEMP) stars, possiblerelics of the early Universe. The chemically anomalous abundance patterns([C/Fe] $\geq$ 0.7) in this subset of low-mass stars suggest pollution byprimordial core-collapsing supernovae (SNe) ejecta that are particularly richin carbon dust grains. By comparing the dust-settling timescale in theprotoplanetary disks of CEMP stars to the expected disk lifetime (assumingdissipation via photoevaporation), we determine the maximum distance $r_{max}$from the host CEMP star at which carbon-rich planetesimal formation ispossible, as a function of the host star's [C/H] abundance. We then use ourlinear relation between $r_{max}$ and [C/H], along with the theoreticalmass-radius relation derived for a solid, pure carbon planet, to characterizepotential planetary transits across host CEMP stars. Given that the relatedtransits are detectable with current and upcoming space-based transit surveys,we suggest initiating an observational program to search for carbon planetsaround CEMP stars in hopes of shedding light on the question of how earlyplanetary systems may have formed after the Big Bang.

CEMP stars: possible hosts to carbon planets in the early universe