Abstract
ABSTRACT HD154708 has an extraordinarily strong magnetic field of 24.5kG. Using 2.5h of high timeresolution Ultraviolet and Visual Echelle Spectrograph (UVES) spectra we have discoveredthis star to be an roAp star with a pulsation period of 8min. The radial velocity amplitudes intherareearthelementlinesofNd II ,Nd III andPr III areunusuallylow–∼60ms −1 –foranroApstar.SomeevidencesuggeststhatroApstarswithstrongermagneticfieldshavelowerpulsationamplitudes. Given the central role that the magnetic field plays in the oblique pulsator modelof the roAp stars, an extensive study of the relation of magnetic field strength to pulsationamplitude is desirable. Key words: stars: individual: HD154708 – stars: magnetic fields – stars: oscillations – stars:variables: other. 1 INTRODUCTION ThemagneticAstarsareimportantforthestudyoftheinteractionofstellar magnetic fields with rotation, pulsation and atomic diffusion,allofwhichhaveimplicationsformanyfieldsofstellarastrophysics.As with many physical systems, extreme cases may provide tests ofour understanding of these systems. Recently Hubrig et al. (2005)discovered one of the strongest magnetic fields known for an uppermain sequence chemically peculiar star,
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