XUV LINES EMITTED FROM PLASMA ACCELERATED DURING MAGNETIC RECONNECTION

We compute the intensity of the emission in the O VI, Mg X, Si XII, Fe XIII, Fe XVI transitions and the profiles of these spectral lines for a plasma flowing out of reconnecting current sheets that originate in the active region corona either during transient brightenings or in p reflare conditions. The characteristic of these lines is a significant non-thermal broadening consistent with plasma non-thermal velocities of the order of 300 km s(-1). Hence, it is possible to infer the occur rence of magnetic reconnection in the solar corona by investigating th e broadening of transition region and coronal lines in the sites where reconnection is presumed to take place.