PHysics of Oscillating STars
Published December 13, 2018 | Version v1
Conference paper Open

PB 8783: the first sdO star suitable for asteroseismic modeling?

Creators

  • 1. Université de Liège
  • 2. ESO Garching
  • 3. Universität Göttingen
  • 4. Astronomical Institute of the Czech Academy of Sciences; Astroserver.org
  • 5. Université de Montréal
  • 6. IRAP - Université de Toulouse - CNRS
  • 7. Steward Observatory, University of Arizona

Contributors

  • 1. IRAP - Université de Toulouse - CNRS

Description

Pulsating hot B subdwarfs (sdB) have become one of the showcases of asteroseismology. Thanks to the combination of rich observed pulsation spectra and state-of-the-art modeling tools it is possible to tightly constrain fundamental parameters such as the stellar mass for these compact, evolved objects in the core He-burning phase of evolution. In comparison, the exploitation of sdO pulsators - hotter stars thought to be in a more advanced evolutionary stage - is still in its infancy. While a small number have been identified in Globular Clusters (GCs), they are extremely rare among the field population. It was recently suggested that PB8783, one of the very first sdB pulsators discovered in 1997, may in fact be an unrecognized hot sdO star with very similar properties to the GC sdO pulsators. Here, we present new very high-quality spectroscopy as well as an asteroseismic analysis of this star with the aim of solving the mystery of its nature.

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