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Time-resolved high-resolution spectroscopy
of the bright
sdBV Balloon090100001
John Telting et al., Bamberg, July 2007
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Seismology of stars; need for accurate mode identification
Seismologogy probes the inner
structure of stars, and can/may provide clues to the general
evolution of subdwarf OB stars
Observations reveal eigenvalues
(pulsation frequencies), and eigenfunctions (pulsation modes), and
basic stellar parameters
Asteroseismological analyses
benefit from observed frequencies and observed
mode-identifications to conclusively constrain the internal structure.
It is suggested to provide observational constraints on the pulsation
modes to aid the asteroseismological analyses (e.g. Charpinet et al
2005; PG1219).
Complementary observational
techniques to identify pulsation modes:
-
photometric/spectroscopic amplitude ratios ⇒ probes temperature,
gravity, radial velocity ⇒ gives L
(Baran/Oreiro
today; Fontaine poster) Needs non-adiabatic modeling!
- line-profile variability ⇒ probes 3D velocity field ⇒
gives L and |M| (Schoenaers today)