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The young, rapidly rotating Bp star HR5624 (HD133880) shows an unusuallystrong non-sinusoidal variability of its longitudinal magnetic field. Thisbehaviour was previously interpreted as the signature of an exceptionallystrong, quadrupole-dominated surface magnetic field geometry. We studied themagnetic field structure and chemical abundance distributions of HR5624 withthe aim to verify the unusual quadrupolar nature of its magnetic field and toinvestigate correlations between the field topology and chemical spots. Weanalysed high resolution, time series Stokes parameter spectra of HR5624 withthe help of a magnetic Doppler imaging inversion code based on detailedpolarised radiative transfer modelling of the line profiles. Our magneticDoppler inversions reveal that the field structure of HR5624 is considerablysimpler 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 4kG. Our model implies that overall large-scale field topology of HR5624 isbetter described as a distorted, asymmetric dipole. The chemical abundance mapsof Mg, Si, Ti, Cr, Fe, and Nd obtained in our study are characterised bylarge-scale, high-contrast abundance patterns. These structures correlateweakly with the magnetic field geometry and show no distinct elementconcentrations in the horizontal field regions predicted by theoretical atomicdiffusion calculations. We conclude that the surface magnetic field topology ofHR5624 is not as unusual as previously proposed. Considering these resultstogether with other recent magnetic mapping analyses of early-type starssuggests that predominantly quadrupolar magnetic field topologies, invoked tobe present in a significant number of stars, probably do not exist in realstars.

Magnetic field topology and chemical abundance distributions of the young, rapidly rotating chemically peculiar star HR5624