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 present the first extensive seismic modelling of SX Phe stars in thestellar system $\omega$ Cen. First, using the new values of reddening $E(B-V)$and distance modulus $(m-M)_V$, and bolometric corrections from Kurucz modelatmospheres, we determine the effective temperatures and luminosities of all SXPhe variables in $\omega$ Cen with available $(B-V)$ colours. Next, wecarefully select SX Phe stars that have a frequency ratio strongly suggestingexcitation of two radial modes, and, in addition, their preliminary pulsationalmodels have the values of $(T_{\rm eff},~ L)$ consistent with observationaldeterminations. For five double-mode radial pulsators, we perform an extensiveseismic modeling using the Bayesian analysis based on Monte Carlo simulations.We study the effect of opacity tables and helium abundance. With the OPAL dataand $Y=0.30$, we obtained masses in the range (1.0,~1.2) M$_{\odot}$,metallicity $Z\in(0.0007,~0.0029)$ and the age of about (1.9,~3.8) Gyr. The OPand OPLIB seismic models have always higher metallicites, sometimes outside theallowed range for $\omega$ Cen. In the case of three stars, we find seismicmodels within the observed range of $(T_{\rm eff},~L)$ with all three opacitytables. In the case of two stars, with the highest metallicity, seismic modelscomputed with the OP and OPLIB tables are located far outside the observederror box. The OPAL seismic models follow the age$-$metallicity relation knownfor $\omega$ Cen from the literature.

Asteroseismology of blue stragglers in $\omega$ Centauri: the case of five double-mode radial SX Phoenicis pulsators