The curious case of HCO$^+$: Extreme abundances under extreme conditions

Abstract: Context. HCO$<sup>+$ is widely observed in both Galactic and extragalactic environments and typically exhibits abundances of $10<sup>{-9}-10<sup>{-8}$. However, recent modeling studies suggest that in environments exposed to elevated cosmic-ray ionization rates and strong thermal or mechanical processing its abundance may increase by several orders of magnitude. Aims. To interpret these predictions, we need to understand the physical conditions that produce extreme HCO$<sup>+$ abundances and the chemical pathways that drive these enhancements. Methods. We used UCLCHEM, a gas-grain chemical code, to model the chemistry of HCO$<sup>+$ in dense molecular, protostellar, and shocked gas under elevated cosmic-ray ionization rates ($ζ\ge 10<sup>{-15}\,\mathrm{s<sup>{-1}}$). Results. Extreme HCO$<sup>+$ enhancements leading to $X$(HCO$<sup>+$) $\gtrsim 10<sup>{-4}$ occur only under specific combinations of temperature, density, and cosmic-ray ionization rate, primarily in protostellar and shocked gas. Increasing density generally suppresses the peak HCO$<sup>+$ abundance, requiring higher ionization rates to produce comparable enhancements. More importantly, the extreme enhancements seem to be very dependent on the chemical network used (in our case UMIST12 versus UMIST22, with the latter leading to extreme abundances). These differences among networks arise from the removal of the destruction pathway of HCO$<sup>+$: C + HCO$<sup>+$ $\rightarrow$ CO + CH$<sup>+$, and propagate to several other species including N$_2$H$<sup>+$, H$_2$O, and H$_3$O$<sup>{+}$.