As pointed out by Winget et al. (1994) and Vuille et al. (2000),
the observed triplets in the 1900 and 1994 data sets had
splittings ranging from 6.5
Hz from the "external'' modes
(such as k=17) to 3.6
Hz for the "internal'' modes
k=8 and 9.
Winget et al. interpreted these splittings to be the result of
radial differential rotation, and Kawaler et al. (1999) examined
this interpretation in more detail.
An examination of the frequencies found in the 2000 data set,
shown in Table 9, shows that the multiplet structure
is much harder to discern, since the k=10 through 20 modes typically
have only one multiplet member with a large amplitude.
The obvious multiplet members have frequencies that agree with the
1990 data, except for the 16- mode, where there is a
Hz
shift in the 2000 data.
Note that the k=10 mode identified at
is different than the
identified by Winget et al. (1994) in the 1990 data.
However, the
peak they identified is not the highest peak in that region of the Fourier
transform (see Fig. 13).
Our analysis of the 1990 data has statistically significant k=10peaks close to
Hz and 2008
Hz.
The only modes with obvious multiplet structure
are the k=9 mode, which still shows an obvious
3.6
Hz split triplet, and
the k=8 mode, which shows two peaks that are
consistent with
Hz separation.
In Table 11 we have a peak 3.3
Hz from the k=15, m=1mode that we have not seen before; we call it the 15b mode.
We are not certain whether this is another member of the k=15 multiplet
(analogous to the 15a mode in the 1994 WET data) or if it is
something else.
The 1994 data set also presented a large peak 4.4
Hz
from k=15, m=0, which we call the 15a mode, in addition to the
components. We have not seen this 15a mode in any other
data set other than the 1994 WET run.
The identity of the "extra subcomponents'' remains an unsolved mystery.
Copyright ESO 2003