  This work is devoted to study the magnetic reconnection instability under
solar spicule conditions. Numerical study of the resistive tearing instability
in a current sheet is presented by considering the magnetohydrodynamic (MHD)
framework. To investigate the effect of this instability in a stratified
atmosphere of solar spicules, we solve linear and non-ideal MHD equations in
the x-z plane. In the linear analysis it is assumed that resistivity is only
important within the current sheet, and the exponential growth of energies
takes place faster as plasma resistivity increases. We are interested to see
the occurrence of magnetic reconnection during the lifetime of a typical solar
spicule.
