The effective temperatures were estimated using the Strömgren photometric
indices (available for the program stars through the WEBDA data base, see
Mermilliod 1999) by means of the numerical code written by T.T. Moon
(based on the grid published in Moon & Dworetsky 1985) and
modified by Napiwotzki (1994). In the WEBDA data base, however,
the -index is given for only two of our program stars. For the
remaining ones we used either the measurements given in the paper of
Schönberner & Napiwotzki (1994), or obtained by Schönberner
(unpublished) with the same technique as explained in Schönberner &
Napiwotzki (1994).
In cases where H
and H
profiles were available (cf. Table 1)
the gravities were specified by matching observed and calculated
profiles. The profiles of the hydrogen lines were calculated with the help
of the SYNSPEC code (Hubeny et al. 1994).
For K88, K316 and K1270 hydrogen profiles are not available, and we used
gravities determined by photometry. However, for K316 and K1270 the
photometrically determined gravities appeared to be inconsistent with their
positions in the HR diagram (see Fig. 4 from Breger 1982).
For the less evolved star, K316, we adopted
,
and for K1270
.
Note that these adopted gravities differ
0.4 dex from the
photometrically estimated ones, but this difference has a small influence
on the derived abundances in the temperature region in question.
The finally adopted effective temperatures and gravities are collected in Table 2. Note that for K409, K677, K1211 and Vega the values given in Schönberner & Napiwotzki (1994) were used.
Projected rotational velocities were determined by matching observed and calculated profiles of the hydrogen and/or metallic lines (mainly Mgii) and are also listed in Table 2.
Knum |
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K88 | 8900 | 3.7 | 80 |
K316 | 8950 | 4.0 | 25 |
K371 | 8500 | 3.7 | 45 |
K409 | 9480 | 4.2 | 140 |
K677 | 10680 | 3.6 | 40 |
K746 | 8600 | 3.5 | 20 |
K1211 | 12630 | 3.6 | 30 |
K1270 | 8300 | 3.5 | 25 |
Vega | 9500 | 4.0 | 22 |
Copyright ESO 2001