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