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 Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

The information on stellar parameters and on the stellar interior we can getby studying pulsating stars depends crucially on the available observationalconstraints: both seismic constraints precision and number of detected modes,identification, nature of the modes) and "classical" observations (photosphericabundances, effective temperature, luminosity, surface gravity). We considerthe case of beta Cephei pulsators and, with the aim of estimatingquantitatively how the available observational constraints determine the typeand precision of our inferences, we set the stage for Hare&Hound exercises. Inthis contribution we present preliminary results for one simple case, where weassume as "observed" frequencies a subset of frequencies of a model and thenevaluate a seismic merit function on a dense and extensive grid of models ofB-type stars. We also compare the behaviour of chi^2 surfaces obtained with andwithout mode identification.

Testing the forward approach in modelling beta Cephei pulsators: setting the stage