English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

We aim to perform a theoretical evaluation of the impact of the mass lossindetermination on asteroseismic grid based estimates of masses, radii, andages of stars in the red giant branch phase (RGB). We adopted the SCEPtERpipeline on a grid spanning the mass range [0.8; 1.8] Msun. As observationalconstraints, we adopted the star effective temperatures, the metallicity[Fe/H], the average large frequency spacing $\Delta \nu,$ and the frequency ofmaximum oscillation power $\nu_{\rm max}$. The mass loss was modelled followinga Reimers parametrization with the two different efficiencies $\eta = 0.4$ and$\eta = 0.8$. In the RGB phase, the average error owing only to observationaluncertainty on mass and age estimates is about 8% and 30% respectively. Thebias in mass and age estimates caused by the adoption of a wrong mass lossparameter in the recovery is minor for the vast majority of the RGB evolution.The biases get larger only after the RGB bump. In the last 2.5% of the RGBlifetime the error on the mass determination reaches 6.5% becoming larger thanthe random error component in this evolutionary phase. The error on the ageestimate amounts to 9%, that is, equal to the random error uncertainty. Theseresults are independent of the stellar metallicity [Fe/H] in the exploredrange. Asteroseismic-based estimates of stellar mass, radius, and age in theRGB phase can be considered mass loss independent within the range ($\eta \in[0.0, 0.8]$) as long as the target is in an evolutionary phase preceding theRGB bump.

Theoretical investigation on the mass loss impact on asteroseismic grid-based estimates of mass, radius, and age for RGB stars