Context : Measurements of the fraction of disk-bearing stars in clusters as a function of age indicate protoplanetary disk lifetimes \lesssim 10 Myr .
However , our knowledge of the time evolution of mass accretion in young stars over the disk lifespans is subject to many uncertainties , especially at the lowest stellar masses ( M _ { \star } ) .

Aims : We investigate ongoing accretion activity in young stars in the TW Hydrae association ( TWA ) .
The age of the association ( \sim 8–10 Myr ) renders it an ideal target to probe the final stages of disk accretion , and its proximity ( \sim 50 pc ) enables a detailed assessment of stellar and accretion properties down to brown dwarf masses .

Methods : Our sample comprises eleven TWA members with infrared excess , amounting to 85 % of the total TWA population with disks .
Our targets span spectral types between M0 and M9 , and masses between 0.58 and 0.02 M _ { \odot } .
We employed homogeneous spectroscopic data from 300 to 2500 nm , obtained synoptically with the X-shooter spectrograph , to derive individual extinction , stellar parameters , and accretion parameters for each object simultaneously .
We then examined the luminosity of Balmer lines and forbidden emission lines to probe the physics of the star–disk interaction environment .

Results : Disk-bearing stars represent around 24 % of the total TWA population .
We detected signatures of ongoing accretion for 70 % of our TWA targets for which accurate measurements of the stellar parameters could be derived .
This implies a fraction of accretors of 13–17 % across the entire TWA ( accounting for the disk-bearing , potentially accreting members not included in our survey ) .
The spectral emission associated with these stars reveals a more evolved stage of these accretors compared to younger PMS populations studied with the same instrument and analysis techniques ( e.g. , Lupus ) : ( i ) a large fraction ( \sim 50 % ) exhibit nearly symmetric , narrow H \alpha line profiles ; ( ii ) over 80 % of them exhibit Balmer decrements consistent with moderate accretion activity and optically thin emission ; ( iii ) less than a third exhibit forbidden line emission in [ O I ] 6300Å , indicative of winds and outflows activity ; ( iv ) only one sixth exhibit signatures of collimated jets .
However , the distribution in accretion rates ( \dot { M } _ { acc } ) derived for the TWA sample follows closely that of younger regions ( Lupus , Chamaeleon I , \sigma Orionis ) over the mass range of overlap ( M _ { \star } \sim 0.1–0.3 M _ { \odot } ) .
An overall correlation between \dot { M } _ { acc } and M _ { \star } is detected , best reproduced by the function \dot { M } _ { acc } \propto M _ { \star } ^ { 2.1 \pm 0.5 } .

Conclusions : At least in the lowest M _ { \star } regimes , stars that still retain a disk at ages \sim 8–10 Myr are found to exhibit statistically similar , albeit moderate , accretion levels as those measured around younger objects .
This “ slow ” \dot { M } _ { acc } evolution apparent at the lowest masses may be associated with longer evolutionary timescales of disks around low-mass stars , suggested by the mass-dependent disk fractions reported in the literature within individual clusters .