The Debris Disk Fraction for M-dwarfs in Nearby, Young, Moving Groups

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.