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The production site of gamma-rays in blazar jet is an unresolved problem. Wepresent a method to locate gamma-ray emission region in the framework ofone-zone emission model. From measurements of core-shift effect, the relationbetween the magnetic field strengths ($B'$) in the radio cores of jet and thedistances ($R$) of these radio cores from central supermassive black hole(SMBH) can be inferred. Therefore once the magnetic field strength in gamma-rayemission region ($B'_{\rm diss}$) is obtained, one can use the relation of$B'$-$R$ to derive the distance ($R_{\rm diss}$) of gamma-ray emission regionfrom SMBH. Here we evaluate the lower limit of $B'_{\rm diss}$ by using thecriteria that the optical variability timescale $t_{\rm var}$ should be longeror equal to the synchrotron radiation cooling timescale of the electrons thatemit optical photons. We test the method with the observations of PSK 1510-089and BL Lacertae, and derive $R_{\rm diss}<0.15\delta_{\rm D}^{1/3}(1+A)^{2/3}\$pc for PSK 1510-089 with $t_{\rm var}\sim$ a few hours, and $R_{\rmdiss}<0.003\delta_{\rm D}^{1/3}(1+A)^{2/3}\ $pc for BL Lacertae with $t_{\rmvar}\sim$ a few minutes. Here $\delta_{\rm D} $ is the Doppler factor and $A$is the Compton dominance (i.e., the ratio of the Compton to the synchrotronpeak luminosities).

A Method for Locating High Energy Dissipation Region in Blazar