Spectroscopic Mode Identification in Slowly Pulsating Subdwarf-B Stars

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Mode identification is crucial for an asteroseismological study of any significance. Contrarily to spectroscopic techniques, methods such as period-fitting and multi-colour photometry do not provide a full reconstruction of non-radial pulsations. We present a new method of spectroscopic mode identification and test it on time-series of synthetic spectra appropriate for pulsating subdwarf-B stars. We then apply it to the newly discovered slowly pulsating subdwarf-B star HD 4539.
Presented at the "Third Meeting on Hot Subdwarf Stars and Related Objects"

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Astrophysics

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http://salesiana.dossiersoluciones.com/handle/123456789/159879

Consulte el texto completo en el siguiente enlace:

https://arxiv.org/abs/0804.4355
 http://arxiv.org/abs/0804.4355

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arXiv