Modelling Magnetic Fields in Stars: The Input
Figures
The following figures are Stokes U LSD extracted polarisation profiles
for the described test. All are for the same phase in the star's
rotation. X axis is the spectral abscissa given in velocity units, Y axis is Stokes U
divided by unpolarised continuum intensity, I_c. Lines labelled Class A, Class B, Class C and triplet refer
to profiles extracted using subatlases with different Zeeman patterns.
Figure 1. Rotational velocity 10 km/s. There is a difference
in the profiles extracted using subatlases with different Zeeman
patterns. The profiles cannot be simply scaled into one another.
Figure 2. Rotational velocity 20 km/s. Even neglecting the
"triplet" profile, which is extracted using fewer lines to make the
average, the difference here is
more pronounced than the 10 km/s case.
Figure 3. U profiles extracted using subatlases classed
by line depth, into strong (depth > 0.4) , weak (depth < 0.5) and
intermediate (0.2 < depth < 0.6). Profiles have been scaled to match
near line centre. It is apparent that, especially for strong lines, a
simple multiplicative factor will not scale one profile into the
other.
Back to main section