BREAKDOWN OF THE CORE MASS-LUMINOSITY-RELATION AT HIGH LUMINOSITIES ON THE ASYMPTOTIC GIANT BRANCH

Hot bottom burning in asymptotic giant branch stars causes a breakdown of the core mass-luminosity (M(c)-L) relation. For stellar models with up-to-date input physics, including molecular opacities and the associated higher mixing length, the breakdown takes place at core masses M(c) greater than or similar to 0.85 M., i.e., luminosities brighter than M(bol) approximately -6. This occurs in stars of initial mass greater than or similar to 5 M. for Population I (Z = 0.02) compositions, and greater than or similar to 4 M. for Population II (Z = 0.001). For these stars, the luminosity increases much more steeply than the M(c)-L relation would predict, and is no longer independent of the stellar mass. One obtains behavior ranging from weak mass dependence of the M(c)-L relation as the convective envelope approaches the hydrogen-burning shell, through ever increasing departures from the M(c)-L relation as the convective region penetrates into hydrogen-burning regions (hot bottom burning). Large mass-loss rates (M approximately 3 x 10(-5) M. yr-5) can turn off hot bottom burning by significantly reducing the star's mass (and thus the temperature at the base of the convective envelope), causing the star's luminosity to decline toward the standard M(c)-L relation; such mass-loss rates are still an order of magnitude less than that observed in some OH/IR stars. Uncertainties in molecular opacities can significantly affect the extent of hot bottom burning, and thus the luminosities attained.