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Numerous apparent signatures of magnetic reconnection have been reported inthe solar photosphere, including inverted-Y shaped jets. The reconnection atthese sites is expected to cause localised bi-directional flows and extendedshock waves; however, these signatures are rarely observed as extremely highspatial-resolution data are required. Here, we use H-alpha imaging data sampledby the Swedish Solar Telescope's CRisp Imaging SpectroPolarimeter toinvestigate whether bi-directional flows can be detected within inverted-Yshaped jets near the solar limb. These jets are apparent in the H-alpha linewings, while no signature of either jet is observed in the H-alpha line core,implying reconnection took place below the chromospheric canopy. Asymmetries inthe H-alpha line profiles along the legs of the jets indicate the presence ofbi-directional flows, consistent with cartoon models of reconnection inchromospheric anemone jets. These asymmetries are present for over two minutes,longer than the lifetimes of Rapid Blue Excursions, and beyond \pm 1 \AA\ intothe wings of the line indicating that flows within the inverted-Y shaped jetsare responsible for the imbalance in the profiles, rather than motions in theforeground. Additionally, surges form following the occurrence of theinverted-Y shaped jets. This surge formation is consistent with models whichsuggest such events could be caused by the propagation of shock waves fromreconnection sites in the photosphere to the upper atmosphere. Overall, ourresults provide evidence that magnetic reconnection in the photosphere cancause bi-directional flows within inverted-Y shaped jets and could be thedriver of surges.

Spatially resolved signatures of bi-directional flows observed in inverted-Y shaped jets