LITHIUM PRODUCTION IN HOT ADVECTION-DOMINATED ACCRETION FLOWS IN SOFT-X-RAY TRANSIENTS

High Li abundances have been reported in the late-type secondaries of five soft X-ray transients (SXTs): V404 Cyg, A0620-00, GS 2000+25, Nov a Mus 1991, and Cen X-4. Since Li is likely to be depleted in stars of this type, the origin of the Li is puzzling. Li has not been seen in similar secondaries of cataclysmic variables, which suggests that the high Li abundance is not due to an anomalous suppression of Li depleti on in close binaries. SXTs in the quiescent state have been modeled in terms of hot advection-dominated accretion flows (ADAFs), in which th e ions are essentially at virial temperature. At such temperatures, Li production via a-a spallation is possible. We show that ADAFs can pro duce sufficient Li via spallation to explain the observations in the b lack hole SXTs V404 Cyg, A0620-00, GS 2000 + 25, and Nova Mus 1991. If this explanation is correct, it is the first independent confirmation that accretion flows in quiescent SXTs have a two-temperature plasma with ion temperature much higher than electron temperature. Depending on the Li depletion timescale in the secondary, which may range betwee n 10(7)-10(9) yr, the model requires similar to 10(-4) to 10(-6) of th e accreted mass to be intercepted by the secondary after undergoing Li production and being ejected. In the case of the neutron star SXT, Ce n X-4, we can explain the observed Li only if the mass-accretion rate is similar to 10(-3) times the Eddington rate and if there is enhanced ejection due to a propeller effect. We discuss possible observational tests of this proposal. Li production during outbursts could be quite important and may even dominate over the production during quiescence , but the estimate of the Li yield is uncertain. We calculate the expe cted luminosity in gamma-ray lines due to the production of excited Li and Be nuclei, but conclude that the line cannot be detected with cur rent instruments.