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Magnetic reconnection is a rapid energy release process that is believed tobe responsible for flares on the Sun and stars. Nevertheless, suchflare-related reconnection is mostly detected to occur in the corona, whilethere have been few studies concerning the reconnection in the chromosphere orphotosphere. Here we present both spectroscopic and imaging observations ofmagnetic reconnection in the chromosphere leading to a microflare. During theflare peak time, chromospheric line profiles show significantblueshifted/redshifted components on the two sides of the flaring site,corresponding to upflows and downflows with velocities of $\pm$(70--80) kms$^{-1}$, comparable with the local Alfv\'{e}n speed as expected by thereconnection in the chromosphere. The three-dimensional nonlinear force-freefield configuration further discloses twisted field lines (a flux rope) at alow altitude, cospatial with the dark threads in He I 10830 \r{A} images. Theinstability of the flux rope may initiate the flare-related reconnection. Theseobservations provide clear evidence of magnetic reconnection in thechromosphere and show the similar mechanisms of a microflare to those of majorflares.

Bidirectional outflows as evidence of magnetic reconnection leading to a solar microflare