We present the discoveries of six transiting hot Jupiters : WASP-87b , WASP-108b , WASP-109b , WASP-110b , WASP-111b and WASP-112b .
The planets have masses of 0.51–2.2 M _ { Jup } and radii of 1.19–1.44 R _ { Jup } and are in orbits of 1.68–3.78 d around stars with masses 0.81–1.50 M _ { \odot } .

WASP-111b is in a prograde , near-aligned ( \lambda = -5 \pm 16 ^ { \circ } ) , near-circular ( e < 0.10 at 2 \sigma ) orbit around a mid-F star .
As tidal alignment around such a hot star is thought to be inefficient , this suggests that either the planet migrated inwards through the protoplanetary disc or that scattering processes happened to leave it in a near-aligned orbit .
WASP-111 appears to have transitioned from an active to a quiescent state between the 2012 and 2013 seasons , which makes the system a candidate for studying the effects of variable activity on a hot-Jupiter atmosphere .
We find evidence that the mid-F star WASP-87 is a visual binary with a mid-G star .
Two host stars are metal poor : WASP-112 has [ Fe/H ] = -0.64 \pm 0.15 and WASP-87 has [ Fe/H ] = -0.41 \pm 0.10 .
The low density of WASP-112 ( 0.81 M _ { \odot } , 0.80 \pm 0.04 \rho _ { \odot } ) can not be matched by standard models for any reasonable value of the age of the star , suggesting it to be affected by the “ radius anomaly ” .