Parametric functions of the coronal mass ejection properties close to the Sun based on numerical models

In general, the in situ observation of an interplanetary coronal mass ejection (ICME) is characterized by three different structures: a shock, a compression region and the ICME structure itself. The shock is observed as a discontinuity in the velocity (v), magnetic field (B), density (N) and temperature (T). The compression region is a region in which the N and T are incremented; v and B show high fluctuations. Inside the ICME, the velocity decreases slowly, the N and T are really low. Using HD numerical models, we found the parametric functions which relates the in situ observations with the best set of the CME parameters close to the Sun (remote sensing). This set of data is limited by the error in the respective measurements. In this work, we present the simulations, the parametric method and its application to well documented events. We compare our theoretical predictions with observations at 1 AU.