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Emission mechanisms of the shell-type supernova remnant (SNR) RX J1713.7-3946are studied with multi-wavelength observational data from radio, X-ray, GeV$\gamma$-ray to TeV $\gamma$-ray band. A Markov Chain Monte Carlo method isemployed to explore the high-dimensional model parameter space systematically.Three scenarios for the $\gamma$-ray emission are investigated: the leptonic,the hadronic and a hybrid one. Thermal emission from the background plasma isalso included to constrain the gas density, assuming ionization equilibrium,and a 2$\sigma$ upper limit of about 0.03 cm$^{-3}$ is obtained as far asthermal energies account for a significant fraction of the dissipated kineticenergy of the SNR shock. Although systematic errors dominate the $\chi^2$ ofthe spectral fit of all models, we find that 1) the leptonic model has the bestconstrained model parameters, whose values can be easily accommodated with atypical supernova, but gives relatively poor fit to the TeV $\gamma$-ray data;2) The hybrid scenario has one more parameter than the leptonic one andimproves the overall spectral fit significantly; 3) The hadronic one, which hasthree more parameters than the leptonic model, gives the best fit to theoverall spectrum with relatively not-well-constrained model parameters and veryhard spectra of accelerated particles. The uncertainties of the modelparameters decrease significantly if the spectral indices of acceleratedelectrons and protons are the same. The hybrid and hadronic models also requirean energy input into high-energy protons, which seems to be too high comparedwith typical values of a supernova explosion. Further investigations arerequired to reconcile these observations with SNR theories.

Modeling the Multi-Wavelength Emission of Shell-Type Supernova Remnant RX J1713.7-3946