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Aims. In order to better model massive B-type stars, we need to understandthe physical processes taking place in slowly pulsating B (SPB) stars,chemically peculiar Bp stars, and non-pulsating normal B stars co-existing inthe same part of the H-R diagram.  Methods. We carry out a comparative study between samples of confirmed andwell-studied SPB stars and a sample of well-studied Bp stars with known periodsand magnetic field strengths. We determine their evolutionary state usingaccurate HIPPARCOS parallaxes and Geneva photometry. We discuss the occurrenceand strengths of magnetic fields as well as the occurrence of stellar pulsationamong both groups. Further, we make a comparison of Geneva photometricvariability for both kinds of stars.  Results. The group of Bp stars is significantly younger than the group of SPBstars. Longitudinal magnetic fields in SPB stars are weaker than those of Bpstars, suggesting that the magnetic field strength is an important factor for Btype stars to become chemically peculiar. The strongest magnetic fields appearin young Bp stars, indicating a magnetic field decay in stars at advanced ages.Rotation periods of Bp and pulsation periods of SPB stars are of the same orderand the behaviour of Geneva photometric variability of some Bp stars cannot bedistinguished from the variability of SPB stars, illustrating the difficulty tointerpret the observed variability of the order of days for B-type stars. Weconsider the possibility that pulsation could be responsible for thevariability among chemically peculiar stars. In particular, we show that anon-linear pulsation model is not excluded by photometry for the Bp starHD175362.Comment: Accepted for publication in Astronomy & Astrophysics on 29/01/2007, 8  pages, 9 figure

On the co-existence of chemically peculiar Bp stars, slowly pulsating B stars and constant B stars in the same part of the HR diagram