All Tables

Table 1: Photometric indices and data for HD 92024 (P) and comparison stars. Sources: Kaltcheva (2003) and Shobbrook (1983, for C1).
Table 2: rms scatter of the PMT magnitude differences (mmag) between comparison stars. N is the number of differential measurements.
Table 3: Logbook of the spectroscopic observations of HD 92024. Dates, incl. Julian date (=HJD-2 400 000), indicate start of night in UT. Column 3 lists the observers: Sterken (S), Hensberge (H) and Freyhammer (F). N is the number of spectra obtained that night, $\Delta t_{\rm exp}$ is the mean integration time (s), "Ins'' indicates instrument used (FEROS or ECHELEC) and S/N denotes the range of signal-to-noise at 4500 Å. The last column gives the orbital phase interval covered that night.
Table 4: The effect of prewhitening frequencies in the SAT b light curve, with comparison to the B light curves by EB86. The statistical uncertainty in the errors ( $\sigma$ ) is 10% as derived from observations.
Table 5: Orbital elements for HD 92024.
Table 6: Orbital elements from SBOP fitting to RVs made by cross-correlation of all spectra with the 103-spectrum composite (cf. Table 5). $P=8\hbox{$.\!\!^{\rm d}$ }32457$ . The fitting was made for all RVs (Col. 2) and for nightly averages (Col. 3). In the last column $\sigma$ is rescaled to single velocity measurements for comparison purposes.
Table 7: EW-measurements for HD 92024 FEROS spectra and in model lines for different temperatures and abundances. The second column lists helium abundance for the helium lines (using $\log g=3.8$ ) and metal abundance for selected metal lines ( $\log g=4.0$ ), while Cols. 3-5 give corresponding model EWs for three different temperatures. The last columns give EWs for the two composite spectra, combined from all 103, and from 10 similar spectra.
Table 8: Velocity shifts for selected lines in the 103-spectrum composite. Error estimates are deduced from fitting same profiles with different fitting parameters (see text), and the listed shifts are means of the three measurements. Laboratory wavelengths are from Martin et al. (1999). Last column: comments on line strength and profile.
Table 9: Wilson-Devinney binary model solutions for the 4 light curves and model RVs for HD 92024. $k=r_{\rm B}/r_{\rm A}$ . Assumed were e=0.028, $\omega =64\hbox {$^\circ $ }$ , q=0.20, $T_{\rm eff,A}=$ 25 500 K and $i=85\hbox{$.\!\!^\circ$ }2$ . Stellar radii $r_{\rm A,B}$ are in units of the orbital semi-major axis a. ${\mathcal L}_{\rm A,B}(\phi_{0.25})$ are the normalised ( ${\mathcal L}_{\rm A}(\phi_{0.25})+ {\mathcal L}_{\rm B}(\phi_{0.25})\equiv 1$ ) light contributions at phase 0.25. Last row gives number of observations for light curves and RVs.
Table 10: Mean elements for HD 92024. $T_{\rm eff,A}$ = 25 500.
Table 11: Wilson-Devinney binary model solution for HD 92024 for fixed mean geometry from Table 9. q = 0.20 and $T_{\rm eff,A}=25~500$ K. The resulting mean temperature is $\langle T_{\rm eff,B}\rangle =12~410\pm860$ K.
Table 12: Astrophysical data for HD 92024. $M_{\rm bol,\odot } =4.75$ is assumed, and $M_{\odot } = 1.989\times 10^{30}$ kg and $G= 6.67259\times 10^{-11}$ m³ kg^-1 s^-2 are from Seidelmann (1992). Bolometric corrections are from Flower (1996).