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Aims. We gathered about 100 high-resolution spectra of three typical HgMn(mercury-manganese) stars, HD 11753, HD 53244, and HD 221507, to search forslowly pulsating B-like pulsations and surface inhomogeneous distribution ofvarious chemical elements. Methods. Classical frequency analysis methods wereused to detect line profile variability and to determine the variation period.Doppler imaging reconstruction was performed to obtain abundance maps ofchemical elements on the stellar surface. Results. For HD 11753, which is thestar with the most pronounced variability, distinct spectral line profilechanges were detected for Ti, Sr, Y, Zr, and Hg, whereas for HD 53244 and HD221507 the most variable line profiles belong to the elements Hg and Y,respectively. We derived rotation periods for all three stars from thevariations of radial velocities and equivalent widths of spectral linesbelonging to inhomogeneously distributed elements: P_rot (HD 11753)=9.54 d,P_rot (HD 53244)=6.16 d, and P_rot (HD 221507)=1.93 d. For HD 11753 the Dopplerimaging technique was applied to derive the distribution of the most variableelements Ti, Sr, and Y using two datasets separated by ~65 days. Results ofDoppler imaging reconstruction revealed noticeable changes in the surfacedistributions of TiII, SrII, and YII between the datasets, indicating thehitherto not well understood physical processes in stars with radiativeenvelopes that cause a rather fast dynamical chemical spot evolution.

Dynamical evolution of titanium, strontium, and yttrium spots on the surface of the HgMn star HD 11753