  I present the first substantial work to measure the fraction of debris disks
for M-dwarfs in nearby moving groups (MGs). Utilising the $AllWISE$ IR catalog,
17 out of 151 MG members are found with an IR photometric excess indicative of
disk structure. The M-dwarf debris disk fraction is $\lesssim 6$ per cent in
MGs younger than 40\,Myr, and none are found in the groups older than 40\,Myr.
Simulations show, however, that debris disks around M-dwarfs are not present
above a $WISE$ $W1-W4$ colour of $\sim 2.5$, making calculating the absolute
disk fractions difficult. The debris disk dissipation timescale appears to be
faster than for higher-mass stars, and mechanisms such as enhanced stellar wind
drag and/or photoevaporation could account for the more rapid decline of disks
observed amongst M-dwarfs.
