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A MAGNETIC MODEL FOR THE AP STAR HD 192678

We present a magnetic model for the A2pCr star HD 192678 based upon modeling of new and previously published longitudinal magnetic eld measurements, surface eld measurements, broadband linear polarimetry and unpolarized high-resolution spectra. The limitations of the classical dipole oblique rotator model are clearly detectable in the case of HD 192678. An oblique rotating dipole is not capable of simultaneously reproducing the surface eld variations and the broadband linear polarization variations. Line proole variations of the Fe II 6149:2 Zeeman doublet may be consistent with a dipole eld whose pole-to-equator modulus ratio has been decreased by about 20%. However, this is uncertain since it relies critically on the amount of microturbulence present, about which we have little information. Excess broadening of Fe II 6149:2 is apparent which appears to be neither rotational nor microturbulent in origin, and may be indicative of small photospheric regions of high eld strength. Our magnetic model for HD 192678 consists of an oblique rotating dipole with modiied eld line inclinations. The polar eld strength of the dipole is 6:80:2 kG, with i = 173 5 and = 120 7. This model contains a region of open eld lines near the magnetic equator, a recurring feature in magnetic models of a number of Ap stars (Leroy et al. 1995b).