CO2 binding energies on water ice follow a bimodal Gaussian distribution that significantly extends the gaseous CO2 fraction in protoplanetary disks.
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3 Pith papers cite this work. Polarity classification is still indexing.
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Pith papers citing it
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Radiative transfer modeling of protostellar ices shows absorption originates mainly from 1000-2000 au at the cavity-envelope transition, with apparent CO2/H2O and CO/H2O ratios potentially underestimated due to line-of-sight effects.
JWST photometry detects CO, H2O, and CO2 ices in Galactic Center clouds, with >25% of carbon frozen in CO ice implying Z_GC ≳2.5 Z_⊙ under equal freezeout assumption.
citing papers explorer
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Fizzy water ice in space: CO$_2$ adsorption, binding energies and its fate in a protoplanetary disk
CO2 binding energies on water ice follow a bimodal Gaussian distribution that significantly extends the gaseous CO2 fraction in protoplanetary disks.
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CORINOS V: Radiative transfer effects in protostellar ice observations
Radiative transfer modeling of protostellar ices shows absorption originates mainly from 1000-2000 au at the cavity-envelope transition, with apparent CO2/H2O and CO/H2O ratios potentially underestimated due to line-of-sight effects.
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The Colors of Ices: Measuring ice column density through photometry
JWST photometry detects CO, H2O, and CO2 ices in Galactic Center clouds, with >25% of carbon frozen in CO ice implying Z_GC ≳2.5 Z_⊙ under equal freezeout assumption.