Pulsational instability of high-luminosity H-rich pre-white dwarf star

Leila M. Calcaferro; Alejandro H. Córsico; María E. Camisassa; Leandro G. Althaus; Hiromoto Shibahashi

doi:10.1051/epjconf/201715206012

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Proceedings

Open Access

EPJ Web of Conferences 152, 06012 (2017)
https://doi.org/10.1051/epjconf/201715206012

Pulsational instability of high-luminosity H-rich pre-white dwarf star

Leila M. Calcaferro¹^,2^*, Alejandro H. Córsico¹^,2^**, María E. Camisassa¹^,2^***, Leandro G. Althaus¹^,2^**** and Hiromoto Shibahashi³^†

¹ Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Paseo del Bosque s/n, (1900) La Plata, Argentina
² Instituto de Astrofísica La Plata, CONICET-UNLP, Paseo del Bosque s/n, (1900) La Plata, Argentina
³ Department of Astronomy, The University of Tokyo, Japan

^* lcalcaferro@fcaglp.unlp.edu.ar
^** acorsico@fcaglp.unlp.edu.ar
^*** camisassa@fcaglp.unlp.edu.ar
^**** althaus@fcaglp.unlp.edu.ar
^† shibahashi@astron.s.u-tokyo.ac.jp

Published online: 8 September 2017

Abstract

We present a pulsational stability analysis on high-luminosity H-rich (DA) white dwarf models evolved from low-metallicity progenitors. We found that the ε mechanism due to H-shell burning is able to excite low-order g modes.

© The Authors, published by EDP Sciences, 2017

This is an Open Access article distributed under the terms of the Creative Commons Attribution License 4.0, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.