PRELIMINARY WORK:
Spectroscopic Binary
ADOPTED PARAMETERS:
Primary: HgMn star
Teff=11000K, logg=3.80; vturb=0.0 km/s, vsini=1.0 km/s, AT12
Adgiustment of parameters from Stromgren photometry (11100,3.8) in order to
fit Hbeta and get Fe I.Fe II ionization equilibrium.
Secondary:
Teff=8750 K (from DV) logg=4.0 (assumed), vsini=200 km/sec (from Mg II, 4481)
L(A)=63% L(B)=37% from the ratio of model fluxes.
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(Dolk et al. 2002, A&A 385,111 used:
Primary:
Teff=11088K, logg=3.79 from Stromgren photometry as a single star,
vturb=0.0 km/s, vsini=2.0 km/s
Secondary:
Teff=8500 K, logg=4.0, vsini=50 km/sec
L(A)/L(B)=4. )
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Primary:
No solar abundances: He -1.70 [-0.65]
C -4.12 [-0.60]
N <-5.62 <[-1.50]
O -3.70 [-0.49]
Mg -5.06 [-0.60]
Al -7.17 [-1.60]
Si -5.30 [-0.81]
P -6.00 [+0.59]
S -5.21 [-0.50]
Ca -5.83 [-0.15]
V -9.44 [-1.40]:
Cr -5.80 [+0.57]
Mn -5.00 [+1.65]
Ni -6.79 [-1.00]
Sr -7.07 [+2.00]
Y -5.95 [+3.85]
Zr -8.20 [+1.24]
Xe -6.00 [+3.87]
Pr -9.50 [+1.80]
Nd -9.14 [+1.40]
Yb -8.11 [-2.85]
Pt -6.70 [+3.54] isotopic anomaly
Au -7.23 [+3.80]
Hg -5.70 [+5.25] isotopic anomaly
Ca II infrared triplet: Dlam=+0.17, 0.18, 0.18
Pt 194 0% terrest. 32.9%
195 0% 33.8%
196 0% 25.2%
198 100% 7.19%
Hg 196 0% terrest. 0.1534%
198 0.16% 9.968 %
199 0.76% 16.873%
200 2.97% 23.096%
201 4.83% 13.181%
202 50.58% 29.863%
204 40.74% 6.865%
Secondary: solar abundances