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The star formation in molecular clouds is inefficient. The ionizing EUVradiation ($h \nu \geq 13.6$ eV) from young clusters has been considered as aprimary feedback effect to limit the star formation efficiency (SFE). We herefocus on effects of the stellar FUV radiation (6 eV $\leq h \nu \leq$ 13.6 eV)during the cloud disruption stage. The FUV radiation may further reduce the SFEvia photoelectric heating, and it also affects the chemical states of the gasthat is not converted to stars ("cloud remnants") via photodissociation ofmolecules. We have developed a one-dimensional semi-analytic model whichfollows the evolution of both the thermal and chemical structure of aphotodissociation region (PDR) during the dynamical expansion of an HII region.We investigate how the FUV feedback limits the SFE, supposing that the starformation is quenched in the PDR where the temperature is above a thresholdvalue (e.g., 100K). Our model predicts that the FUV feedback contributes toreduce the SFEs for the massive ($M_{\rm cl} \gtrsim 10^5 M_{\odot}$) cloudswith the low surface densities ($\Sigma_{\rm cl} \lesssim 100$M$_{\odot}$pc$^{-2}$). Moreover, we show that a large part of the H$_2$molecular gas contained in the cloud remnants should be "CO-dark" under the FUVfeedback for a wide range of cloud properties. Therefore, the dispersedmolecular clouds are potential factories of the CO-dark gas, which returns intothe cycle of the interstellar medium.

Factories of CO-dark gas: molecular clouds with limited star formation efficiencies by FUV feedback