The role of asteroseismology in understanding mass-loss in red giants

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ABSTRACT Red giant stars play a key role in advancing our understanding of stellar mass-loss. However, its initial mass and the amount of mass lost during this phase remain uncertain. In this study, we investigate the asteroseismic signatures of mass-loss and the parameters that influence it. We examine six stars identified as red giant branch (RGB) stars in the APOKASC-2 catalogue. Assuming these stars are on their first ascent of the RGB, we construct interior models. The resulting model ages are significantly older than the age of the Galaxy, indicating that these stars are likely experiencing mass-loss and evolving toward the red clump (RC) phase. The minimum possible initial masses are estimated using the mass-metallicity diagram, from which we infer that the minimum mass lost by these stars ranges from 0.1–$0.3\, {\rm M}_{\odot }$. Models constructed with an initial minimum mass yield the maximum possible age of the star. The ages of these models fall within the range of 9–9.5 Gyr. For two stars, asteroseismic parameters confirm RC classification. Due to degeneracies in the HR diagram, distinguishing between internal structure models is challenging; however, asteroseismic constraints provide clear differentiation. Although mass-loss and mass-conservation models have similar M, R, and $T_{\rm eff}$ values, $\Delta \nu$s determined from the l = 0 modes in the mass-loss models are 5–10 ${{\ \rm per\ cent}}$ higher than observed. This discrepancy may arise from differences in internal structure. Finally, evolutionary model grids are used to examine how initial mass and Z affect mass-loss. Mass-loss increases with increasing metallicity and decreases with increasing initial mass, regardless of the adopted value of $\eta$.

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