Hostname: page-component-586b7cd67f-l7hp2 Total loading time: 0 Render date: 2024-11-27T20:55:01.141Z Has data issue: false hasContentIssue false
  • English
  • Français

The internal structure of ZZ Cet stars using quantitative asteroseismology: The case of R548

Published online by Cambridge University Press:  18 February 2014

N. Giammichele ,
G. Fontaine ,
P. Brassard  and
S. Charpinet
N. Giammichele
Affiliation:
Département de physique, Université de Montréal, C.P. 6128, Succursale Centre-Ville, Montréal, QC H3C3J7, Canada email: [email protected]
G. Fontaine
Affiliation:
Département de physique, Université de Montréal, C.P. 6128, Succursale Centre-Ville, Montréal, QC H3C3J7, Canada email: [email protected]
P. Brassard
Affiliation:
Département de physique, Université de Montréal, C.P. 6128, Succursale Centre-Ville, Montréal, QC H3C3J7, Canada email: [email protected]
S. Charpinet
Affiliation:
Université de Toulouse, UPS-OMP, IRAP, Toulouse, France; CNRS, IRAP, 14 avenue Edouard Belin, 31400, Toulouse, France
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We explore quantitatively the low but sufficient sensitivity of oscillation modes to probe both the core composition and the details of the chemical stratification of pulsating white dwarfs. Until recently, applications of asteroseismic methods to pulsating white dwarfs have been far and few, and have generally suffered from an insufficient exploration of parameter space. To remedy this situation, we apply to white dwarfs the same double-optimization technique that has been used quite successfully in the context of pulsating hot B subdwarfs. Based on the frequency spectrum of the pulsating white dwarf R548, we are able to unravel in a robust way the unique onion-like stratification and the chemical composition of the star. Independent confirmations from both spectroscopic analyses and detailed evolutionary calculations including diffusion provide crucial consistency checks and add to the credibility of the inferred seismic model. More importantly, these results boost our confidence in the reliability of the forward method for sounding white dwarf internal structure with asteroseismology.

Keywords

stars: oscillationswhite dwarfs
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Symposium S301: Precision Asteroseismology , August 2013 , pp. 285 - 288
Copyright
Copyright © International Astronomical Union 2014 

References

Charpinet, S., Fontaine, G., & Brassard, P. 2009a, A&A, 493, 595Google Scholar
Charpinet, S., Fontaine, G., & Brassard, P. 2009b, Nature, 461, 501Google Scholar
Giammichele, N., Fontaine, G., & Brassard, P. 2013a, European Physical Journal Web of Conferences, 43, 5007Google Scholar
Giammichele, N., Fontaine, G., & Brassard, P. 2013b, ASP-CS, 469, 49Google Scholar
Salaris, M., Cassisi, S., Pietrinferni, A., Kowalski, P. M., & Isern, J. 2010, ApJ, 716, 1241Google Scholar