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Constraints on angular numbers of pulsation modes
from spectroscopy
John Telting, Wrocław, June 2008
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Seismology of stars; need for accurate mode identification
Seismology probes the inner
structure of stars, and can/may provide clues to the general
evolution of 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. For successful applications it is necesary to provide
observational constraints on the pulsation modes to aid the
asteroseismological analyses.
There are two complementary
and independent observational techniques to identify pulsation
modes:
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photometric/spectroscopic amplitude ratios
⇒ probes temperature, gravity, radial velocity
⇒ gives L
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line-profile variability
⇒ probes 3D velocity field
⇒ gives L and M