  Magnetic reconnection modulated by non-local disturbances in the solar
atmosphere has been investigated theoretically, but rarely observed. In this
study, employing Ha and extreme ultraviolet (EUV) images and line of sight
magnetograms, we report acceleration of reconnection by adjacent filament
eruption. In Ha images, four groups of chromospheric fibrils are observed to
form a saddle-like structure. Among them, two groups of fibrils converge and
reconnect. Two newly reconnected fibrils then form, and retract away from the
reconnection region. In EUV images, similar structures and evolution of coronal
loops are identified. Current sheet forms repeatedly at the interface of
reconnecting loops, with width and length of 1-2 and 5.3-7.2 Mm, and
reconnection rate of 0.18-0.3. It appears in the EUV low-temperature channels,
with average differential emission measure (DEM) weighed temperature and EM of
2 MK and 2.5*10^27 cm-5. Plasmoids appear in the current sheet and propagate
along it, and then further along the reconnection loops. The filament, located
at the southeast of reconnection region, erupts, and pushes away the loops
covering the reconnection region. Thereafter, the current sheet has width and
length of 2 and 3.5 Mm, and reconnection rate of 0.57. It becomes much
brighter, and appears in the EUV high-temperature channels, with average
DEM-weighed temperature and EM of 5.5 MK and 1.7*10^28 cm-5. In the current
sheet, more hotter plasmoids form. More thermal and kinetic energy is hence
converted. These results suggest that the reconnection is significantly
accelerated by the propagating disturbance caused by the nearby filament
eruption.
