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Constraints on angular numbers of pulsation modes from spectroscopy John Telting, Wrocław, June 2008 |
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For rotating stars (Veqsin(i) > intrinsic line
broadening) the Doppler-imaging principle applies: the stellar disk is
resolved in the velocity space of the line profile.
Pulsation modes up to L∼20 can be observed
with high-resolution spectroscopy.
| l=0 m=0 radial mode | l=4 m=0 zonal mode | l=5 m=-3 prograde mode | l=9 m=3 retrograde mode | l=7 m=-7 sectoral prograde |
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