The Pulsation of AGB Stars in the Magellanic Cloud Clusters NGC 1978 and NGC 419

TL;DR

This study investigates pulsating AGB stars in the Magellanic Cloud clusters NGC 1978 and NGC 419, deriving their masses, analyzing mass loss rates, and comparing observations with theoretical models to understand stellar evolution.

Contribution

It provides new mass estimates for AGB stars in these clusters and evaluates the accuracy of different mass loss formulas against observed data.

Findings

AGB stars in NGC 1978 have a mass of 1.55Msun

AGB stars in NGC 419 have a mass of 1.87Msun

Vassiliadis & Wood (1993) mass loss formula fits observations well

Abstract

The intermediate-age Magellanic Cloud clusters NGC 1978 and NGC 419 are each found to contain substantial numbers of pulsating AGB stars, both oxygen-rich and carbon-rich. Each cluster also contains two pulsating asymptotic giant branch (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 1.55Msun early on the AGB while the NGC 419 stars have a mass of 1.87Msun early on the AGB. These masses are in good agreement with those expected from the cluster ages determined by main-sequence turnoff fitting. Nonlinear 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 & Wood (1993) reproduce the observations reasonably well. The mass loss rates computed from the formula of Blocker (1995) terminate the AGB in both clusters at a luminosity which is much too low.