Continuous photometry with up to three BRITE satellites was obtained for 12 targets and subjected to a period search. Contemporaneous high-resolution optical spectroscopy with STELLA was used to obtain radial velocities through cross correlation with template spectra as well as to determine astrophysical parameters through a comparison with model spectra. The Capella red light curve was found to be constant over 176 days with a root mean square of 1 mmag, but the blue light curve showed a period of 10.1$pm$0.6 d, which we interpret to be the rotation period of the G0 component. The BRITE light curve of the F0 supergiant $varepsilon$Aur suggests 152 d as its main pulsation period, while the STELLA radial velocities reveal a clear 68 d period. An ingress of an eclipse of the $zeta$Aur binary system was covered with BRITE and a precise timing for its eclipse onset derived. $eta$Aur is identified as a slowly pulsating B (SPB) star with a main period of 1.29 d and is among the brightest SPB stars discovered so far. The rotation period of the magnetic Ap star $theta$Aur is detected from photometry and spectroscopy with a period of 3.6189 d and 3.6177 d, respectively, likely the same within the errors. Photometric rotation periods are also confirmed for the magnetic Ap star $tau$Aur of 2.463 d and for the solar-type star $kappa^1$Cet of 9.065 d, and also for the B7 HgMn giant $beta$Tau of 2.74 d. Revised orbital solutions are derived for the eclipsing SB2 binary $beta$Aur, for the 27 year eclipsing SB1 $varepsilon$Aur, and for the RS CVn binary HR 1099. The two stars $ u$ Aur and $iota$Aur are found to be long-term, low-amplitude RV and brightness variables, but provisional orbital elements based on a period of 20 yr and an eccentricity of 0.7 could only be extracted for $ u$Aur. The variations of $iota$Aur are due to oscillations with a period of $approx$4 yr.
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