  The young, rapidly rotating Bp star HR5624 (HD133880) shows an unusually
strong non-sinusoidal variability of its longitudinal magnetic field. This
behaviour was previously interpreted as the signature of an exceptionally
strong, quadrupole-dominated surface magnetic field geometry. We studied the
magnetic field structure and chemical abundance distributions of HR5624 with
the aim to verify the unusual quadrupolar nature of its magnetic field and to
investigate correlations between the field topology and chemical spots. We
analysed high resolution, time series Stokes parameter spectra of HR5624 with
the help of a magnetic Doppler imaging inversion code based on detailed
polarised radiative transfer modelling of the line profiles. Our magnetic
Doppler inversions reveal that the field structure of HR5624 is considerably
simpler and the field strength is much lower than proposed by previous studies.
We find a maximum local field strength of 12 kG and a mean field strength of 4
kG. Our model implies that overall large-scale field topology of HR5624 is
better described as a distorted, asymmetric dipole. The chemical abundance maps
of Mg, Si, Ti, Cr, Fe, and Nd obtained in our study are characterised by
large-scale, high-contrast abundance patterns. These structures correlate
weakly with the magnetic field geometry and show no distinct element
concentrations in the horizontal field regions predicted by theoretical atomic
diffusion calculations. We conclude that the surface magnetic field topology of
HR5624 is not as unusual as previously proposed. Considering these results
together with other recent magnetic mapping analyses of early-type stars
suggests that predominantly quadrupolar magnetic field topologies, invoked to
be present in a significant number of stars, probably do not exist in real
stars.
