We explore the shock acceleration model for giant radio relics, in which relativistic electrons are accelerated via diffusive shock acceleration (DSA) by merger-driven shocks in the outskirts of galaxy clusters. In addition to DSA, turbulent acceleration by compressive MHD modes downstream of the shock are included as well as energy losses of postshock electrons due to Coulomb scattering, synchrotron emission, and inverse Compton scattering off the cosmic background radiation. Considering that only a small fraction of merging clusters host radio relics, we favor a reacceleration scenario in which radio relics are generated preferentially by shocks encountering the regions containing low-energy ( e . 300) cosmic ray electrons (CRe). We perform time-dependent DSA simulations of spherically expanding shocks with physical parameters relevant for the Sausage radio relic, and calculate the radio synchrotron emission from the accelerated CRe. We find that significant level of postshock turbulent acceleration is required in order to reproduce broad profiles of the observed radio flux densities of the Sausage relic. Moreover, the spectral curvature in the observed integrated radio spectrum can be explained, if the putative shock should have swept up and exited out of the preshock region of fossil CRe about 10~Myr ago.

Abstract
1. INTRODUCTION
2. NUMERICAL CALCULATIONS
    2.1. DSA Simulations for 1D Spherical Shocks
    2.2. Injection versus ReaccelerationModel
    2.3. Shock Parameters
3. RESULTS OF DSA SIMULATIONS
    3.1. Surface Brightness and Spectral Index Profiles
    3.2. Integrated Spectrum
4. SUMMARY
REFERENCES

• Hyesung Kang(Department of Earth Sciences, Pusan National University) Corresponding author