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

TL;DR

This paper explores the effectiveness of the forward modelling approach for beta Cephei pulsators by analyzing how observational constraints influence stellar parameter inference, using Hare&Hound exercises and seismic merit functions.

Contribution

It introduces a framework for assessing the impact of observational data on seismic modelling accuracy for beta Cephei stars, including preliminary results and comparison of chi^2 surfaces with mode identification.

Findings

Seismic constraints significantly affect parameter inference accuracy.

Mode identification improves the shape of chi^2 surfaces.

Preliminary results demonstrate the potential of the forward approach.

Abstract

The information on stellar parameters and on the stellar interior we can get by studying pulsating stars depends crucially on the available observational constraints: both seismic constraints precision and number of detected modes, identification, nature of the modes) and "classical" observations (photospheric abundances, effective temperature, luminosity, surface gravity). We consider the case of beta Cephei pulsators and, with the aim of estimating quantitatively how the available observational constraints determine the type and precision of our inferences, we set the stage for Hare&Hound exercises. In this contribution we present preliminary results for one simple case, where we assume as "observed" frequencies a subset of frequencies of a model and then evaluate a seismic merit function on a dense and extensive grid of models of B-type stars. We also compare the behaviour of chi^2 surfaces obtained with and without mode identification.