Ellerman bombs and jets associated with resistive flux emergence

Using two-dimensional (2D) magnetohydrodynamic simulations we study the effects of resistive processes in the dynamics of magnetic flux emergence and its relation to Ellerman bombs and other dynamic phenomena in the Sun. The widely accepted scenario of flux emergence is the formation and expansion of Omega-shaped loops due to the Parker instability. Since the Parker instability has the largest growth rate at finite wavelength lambda p similar to 10H-20H, where H is the scale height (approximate to 200 km in the solar photosphere), a number of magnetic loops may rise from the initial flux sheet if it is sufficiently long. This process is shown in our numerical simulations. The multiple emerging loops expand in the atmosphere and interact with each other, leading to magnetic reconnection. At first reconnection occurs in the lower atmosphere, which allows the sinking part of the flux sheet to emerge above the photosphere. This reconnection also causes local heating that may account for Ellerman bombs. In the later stage, reconnection between the expanding loops occurs at higher levels of the atmosphere and creates hightemperature reconnection jets, and eventually a large (>>lambda(p)) coronal loop is formed. Cool and dense plasma structures, which are similar to H alpha surges, are also formed. This is not because of magnetic reconnection but due to the compression of the plasma in between the expanding loops.