Solar flare of 5 November 2005 of importance M4.1/1B is investigated. For three moments of this flare (11^h35^m, 11^h39^m and 11h45^m UT), the Stokes I±V profiles of nine lines of Fe I, Fe II, Sc II and Cr II are studied. Magnetic fields in the flare were measured using two methods: 'center of gravity' and on a base of comparison of observed profiles with theoretical ones calculated with Baranovsky's program. There are following from profile's analysis that magnetic field peak had existed in flare maximum (11^h35^m) and placed in the upper photosphere (lgτ₅₀₀ = -2.7). During the flare evolution, this peak became blurred and shifted into deeper layers of the photosphere. Semi-empirical model of the flare has two layers with increased temperature: in upper and middle photosphere. These layers had shifted deeper during flare evolution as well. Turbulent velocities on the maximum of the distribution increased 5 times relatively undisturbed photosphere, whereas plasma density — changed to 3—6 times both to increasing and decreasing.