2019MNRAS.486.1094M

Sources of X-rays such as active galactic nuclei and X-ray binaries are often variable by orders of magnitude in luminosity over time-scales of years. During and after these flares the surrounding gas is out of chemical and thermal equilibrium. We introduce a new implementation of X-ray radiative transfer coupled to a time-dependent chemical network for use in 3D magnetohydrodynamical simulations. A static fractal molecular cloud is irradiated with X-rays of different intensity, and the chemical and thermal evolution of the cloud are studied. For a simulated 10⁵M^_☉fractal cloud, an X-ray flux <0.01 erg cm^–2 s^–1 allows the cloud to remain molecular, whereas most of the CO and H₂ are destroyed for a flux of >=1 erg cm^–2 s^–1. The effects of an X-ray flare, which suddenly increases the X-ray flux by 10⁵x, are then studied. A cloud exposed to a bright flare has 99 per cent of its CO destroyed in 10-20 yr, whereas it takes >10³ yr for 99 per cent of the H₂ to be destroyed. CO is primarily destroyed by locally generated far-UV emission from collisions between non-thermal electrons and H₂; He⁺ only becomes an important destruction agent when the CO abundance is already very small. After the flare is over, CO re-forms and approaches its equilibrium abundance after 10³-10⁵ yr. This implies that molecular clouds close to Sgr A^* in the Galactic Centre may still be out of chemical equilibrium, and we predict the existence of clouds near flaring X-ray sources in which CO has been mostly destroyed but H is fully molecular.