While over 200 planets have been found to orbit F, G and K stars, only 
six have been found around M dwarfs. In spite of their small number, the 
planets identified around very-low-mass stars exhibit some interesting 
statistical properties. In particular, they include no hot-Jupiter and 
very few Jupiter-mass planets at any period. A different frequency of 
Jupiter-mass planets between sun-like stars and M dwarfs may point toward a 
stellar mass dependency in planet formation processes. Our recent work on 
M-dwarf metallicity suggests however that they might have lower abundances 
of heavy elements than earlier-type stars. Given the well established 
overabundance of planets around metal-rich stars, one needs to verify 
whether metallicity alone can explain the statistical properties of M-dwarf 
planets. I will present the emerging properties of planets around M dwarfs, 
and briefly discuss how they mesh up with planet formation theories.