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The intermediate‐age Magellanic Cloud clusters NGC 1978 and 419 are each found to contain substantial numbers of pulsating asymptotic giant branch (AGB) stars, both oxygen rich and carbon rich. Each cluster also contains two pulsating AGB stars which are infrared sources with a large mass‐loss rate. Pulsation masses have been derived for the AGB variables, from the lowest luminosity O‐rich variables to the most evolved infrared sources. It is found that the stars in NGC 1978 have a mass of  1.55 M ⊙   early on the AGB while the NGC 419 stars have a mass of  1.87 M ⊙   early on the AGB. These masses are in good agreement with those expected from the cluster ages determined by main‐sequence turn‐off fitting. Non‐linear pulsation models fitted to the highly evolved AGB stars show that a substantial amount of mass‐loss has occurred during the AGB evolution of these stars. An examination of the observed mass‐loss on the AGB, and the AGB tip luminosities, shows that in both clusters the mass‐loss rates computed from the formula of Vassiliadis &amp; Wood reproduce the observations reasonably well. The mass‐loss rates computed from the formula of Blöcker terminate the AGB in both clusters at a luminosity which is much too low.

The pulsation of AGB stars in the Magellanic Cloud clusters NGC 1978 and 419