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Chemically peculiar (CP) stars of the upper main sequence are characterisedby specific anomalies in the photospheric abundances of some chemical elements.The group of CP2 stars, which encompasses classical Ap and Bp stars, exhibitsstrictly periodic light, spectral, and spectropolarimetric variations that canbe adequately explained by the model of a rigidly rotating star with persistentsurface structures and a stable global magnetic field. Using observations fromthe Kepler K2 mission, we find that the B9pSi star HD 174356 displays a lightcurve both variable in amplitude and shape, which is not expected in a CP2star. Employing archival and new photometric and spectroscopic observations, wecarry out a detailed abundance analysis of HD 174356 and discuss itsphotometric and astrophysical properties in detail. We employ phenomenologicalmodeling to decompose the light curve and the observed radial velocityvariability. Our abundance analysis confirms that HD 174356 is a silicon-typeCP2 star. No magnetic field stronger than 110G was found. The star's lightcurve can be interpreted as the sum of two independent strictly periodicsignals with P1 = 4.04355(5)d and P2 = 2.11169(3)d. The periods have remainedstable over 17 years of observations. In all spectra, HD 174356 appears to besingle-lined. From the simulation of the variability characteristics andinvestigation of stars in the close angular vicinity, we put forth thehypothesis that the peculiar light variability of HD 174356 arises in a singlestar and is caused by rotational modulation due to surface abundance patches(P1) and g mode pulsation (P2).

Rotational modulation and single g-mode pulsation in the B9pSi star HD174356?