In this article we present the O–C diagram of the hot subdwarf B pulsating star HS 2201+2610 after seven years of observations .
A secular increase of the main pulsation period , Ṗ= ( 1.3 \pm 0.1 ) \times 10 ^ { -12 } , is inferred from the data .
Moreover , a further sinusoidal pattern suggests the presence of a low-mass companion ( Msin i \simeq 3.5 M _ { \it Jup } ) , orbiting the hot star at a distance of about 1.7 AU with a period near 1140 days .