Comprehensive stellar seismic analysis : New method exploiting the glitches information in solar-like pulsators. (arXiv:1812.04984v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Farnir_M/0/1/0/all/0/1">M. Farnir</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dupret_M/0/1/0/all/0/1">M-A. Dupret</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Salmon_S/0/1/0/all/0/1">S.J.A.J. Salmon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Noels_A/0/1/0/all/0/1">A. Noels</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Buldgen_G/0/1/0/all/0/1">G. Buldgen</a>
Aims: We develop a method that provides a comprehensive analysis of the
oscillation spectra of solar-like pulsators. We define new seismic indicators
that should be as uncorrelated and as precise as possible and should hold
detailed information about stellar interiors. This is essential to improve the
quality of the results obtained from asteroseismology as it will provide better
stellar models which in turn can be used to refine inferences made in
exoplanetology and galactic archaeology. Methods: The presented method –
WhoSGlAd – relies on Gram-Schmidt’s orthogonalisation process. A Euclidean
vector subspace of functions is defined and the oscillation frequencies are
projected over an orthonormal basis in a specific order. This allows the
obtention of independent coefficients that we combine to define independent
seismic indicators. Results: The developed method has been shown to be stable
and to converge efficiently for solar-like pulsators. Thus, detailed and
precise inferences can be obtained on the mass, the age, the chemical
composition and the undershooting in the interior of the studied stars.
However, attention has to be paid when studying the helium glitch as there
seems to be a degeneracy between the influence of the helium abundance and that
of the heavy elements on the glitch amplitude. As an example, we analyse the
16CygA (HD 186408) oscillation spectrum to provide an illustration of the
capabilities of the method.
Aims: We develop a method that provides a comprehensive analysis of the
oscillation spectra of solar-like pulsators. We define new seismic indicators
that should be as uncorrelated and as precise as possible and should hold
detailed information about stellar interiors. This is essential to improve the
quality of the results obtained from asteroseismology as it will provide better
stellar models which in turn can be used to refine inferences made in
exoplanetology and galactic archaeology. Methods: The presented method –
WhoSGlAd – relies on Gram-Schmidt’s orthogonalisation process. A Euclidean
vector subspace of functions is defined and the oscillation frequencies are
projected over an orthonormal basis in a specific order. This allows the
obtention of independent coefficients that we combine to define independent
seismic indicators. Results: The developed method has been shown to be stable
and to converge efficiently for solar-like pulsators. Thus, detailed and
precise inferences can be obtained on the mass, the age, the chemical
composition and the undershooting in the interior of the studied stars.
However, attention has to be paid when studying the helium glitch as there
seems to be a degeneracy between the influence of the helium abundance and that
of the heavy elements on the glitch amplitude. As an example, we analyse the
16CygA (HD 186408) oscillation spectrum to provide an illustration of the
capabilities of the method.
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