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Based on the method of finding coronal magnetic field value radial profilesB(R) described in (Gopalswamy and Yashiro, 2011), and applied for thedirections close to the sky plane, we determined magnetic field value radialdistributions along the directions close to the Sun-Earth axis. For thispurpose, by using the method in (Xue, Wang, and Dou, 2005), from the SOHO/LASCOdata, we found 3D characteristics for fast halo coronal mass ejections (HCMEs)and for the HCME-related shocks. Through these data, we managed to obtain theB(R) distributions as far as 43 solar radii from the Sun center, which isapproximately by a factor of 2 farther, than those in (Gopalswamy and Yashiro,2011). We drew a conclusion that, to improve the accuracy of theGopalswamy-Yashiro method to find the coronal magnetic field, one shoulddevelop a technique to detect the CME sites that move in the slow and in thefast solar wind. We propose a technique to select the CMEs, whose central(paraxial) part moves, indeed, in the slow wind.

Coronal magnetic field value radial distributions obtained by using the information on fast halo coronal mass ejections