JHT at Wrocław
Constraints on angular numbers of pulsation modes
from spectroscopy
John Telting,   Wrocław,   June 2008
page 05
-5 -1 +1 +5
Introduction:   Pulsational line-profile variability for slowly rotating stars

Low rotational line-broadening ⇒ no Doppler imaging.
   Only L≤4 modes give detectable line-profile variations.

Solution: fit a model of the 3D pulsational surface-velocity field to the observed line-profile variability,     or to the observed velocity moments.
 
L=0 |M|=0 L=1 |M|=1 L=2 |M|=0 L=2 |M|=1 L=2 |M|=2