CORRELATION-FUNCTIONS FOR A RANDOM GALACTIC MAGNETIC-FIELD

We use the anisotropic part of the radio intensity correlation function K2(theta) of the Galactic background for a selected area near the North Galactic Pole (Dagkesamanskii, R. D. and Shutenkov, V. R. (1987). Pis'ma Astron. Zh. 13, 182 [Sov. Astron. Lett. 13, 73 (1987)]) to find the difference between the longitudinal (B(l)(r)) and transverse (B(t)(r)) correlation functions of a random magnetic field. Assuming a solenoidal field, we construct both B(l)(r) and B(t)(r). Those functions are then used to obtain characteristic scales and construct the turbulence spectrum for the random field.