1. XRT and EIS Observations of Reconnection associated Phenomena D. Shiota, H. Isobe, D. H. Brooks, P. F. Chen, and K. Shibata shiota@kwasan.kyoto-u.ac.jp Kwasan and Hida Observatories, Kyoto University, Japan 1.Introduction Magnetic reconnection is widely believed to play an important role in various solar activities such as solar flares, because Yohkoh has observed many peices of evidence for reconnection. However, most of that evidence is indirect and the theory of magnetic reconnection has not been established. Hence our understanding of reconnection is incomplete. Imaging and spectroscopic observations with the EUV Imaging Spectrometer (EIS) and X-ray Telescope (XRT), the new instruments aboard Solar-B, will obtain physical quantities and the spatial structure of the different temperature solar plasmas. This will improve our understanding of the basic processes of magnetic reconnection in the solar tmosphere. In this paper, we present predicted EIS and XRT observations, which are synthesized from the results of 2.5-D magnetohydrodynamic (MHD) simulations of magnetic reconnection, and examine how the reconnection associated phenomena can be observed. 2. MHD simulation 2.5-D time-dependent resistive MHD simulation including heat conduction and gravity. This is a developed model of Chen & Shibata (2000) and Shiota et al. (2005). Initial Parameters Fig. 1 Initial Magnetic configuration and pressure distribution Position of Slit Emission Measure Line of sight Fe XV 284.147 A log(T)=6.30 Fe XV 195.119 A log(T)=6.15 Si VII 275.361 A log(T)=5.75 Ca XVII 192.82 A log(T)=6.70 XRT Thin Al poly image Fig. 2 Left: density distribution at t=50. Solid lines and arrows indicate magnetic field lines and velocity, respectively. Right: temperature distributions at t=50. Solid lines indicate density distribution shown in left panel. Conduction fronts Slow shocks 3. Numerical Results Slow shock 4. Synthesized XRT and EIS observations Inflow behind conduction front Reconnection outflow Inflow outside of conduction front Conduction front inflow Reconnection outflow + conduction front Reconnection outflow Magnetic reconnection occurs below the flux rope. In the inflow region, density and temperature decreases because of the reconnection inflow and rise motion of the flux rope. As the results of reconnection, high temperature upward and downward outflows are generated. The boundaries between inflows and outflows become Petschek-type slow shocks. However, the temperature of the outflow behind the slow shock become so high that the slow shocks are dissociated into conduction fronts and isothermal slow shocks. Behind the conduction front, high temperature inflows exist. Because chromospheric evaporation is not included in the simulation, the cusp-shaped loop is not so realistic. In the next section we examine the observation of X-point. Observations of reconnection associated phenomena Inflow:red and blue shifted components in lower temperature line. Velocity of lower temperature plasma become larger than that of higher temperature plasma. Outflow: red and blue shifted components in higher temperature line. Slow shock: Inflow behind conduction fronts can be observed in higher temperature line. The velocity of the inflow and the outflow are one information of isothermal slow shock. (a) (b)(c)(d) (e) (f) (g) (h) (i) Fig. 3 (a): synthetic XRT image with assumption the simulation data arranged uniformly and we observe from oblique. (b), (d), (f), (g): synthetic EIS spectral image of the indicated four emission lines of the slit shown in (a). (c), (e), (g), (i): emission measure distribution of the each line along the slit and the line of sight.