From four independent calculations using three different theoretical approaches, rate coefficients for the formation of HeH via the radiative association of He and H were computed. Good agreement is found between our new calculations and prior results obtained two decades ago for kinetic temperatures between ∼800 and 20,000 K. This finding is inconsistent with a recent claim in the literature of a wide variation in published values and establishes the robustness of our knowledge of this process for the formation of HeH. The implications of the current results to the first detection of HeH and its modeled abundance in the planetary nebula NGC 7027 are discussed.
