Authors: Carlos Arturo Perez-Alanis (Universidad Nacional Autónoma de México, UNAM), Miho Janvier (Universit ́e Paris-Saclay, CNRS, Institut d’Astrophysique Spatiale, Orsay, France), Teresa Nieves-Chinchilla (Heliophysics Science Division. NASA Goddard Space Flight Center, Greenbelt, MD, USA), Ernesto Aguilar-Rodriguez (Instituto de Geofisica, UNAM), Pascal Dèmoulin (LESIA, Observatoire de Paris, Universitè PSL, CNRS, Sorbonne Universitè, Meudon, France), Pedro Corona-Romero (Catedras CONACyT, UNAM))

In situ observations of interplanetary (IP) coronal mass ejections (ICMEs) and IP shocks are important to study as they are the main components of the solar activity. Hundreds of IP shocks have been detected by various space missions at different times and heliocentric distances. In this study, we carry out a statistical analysis of the distributions of some parameters of the IP shocks. To accomplish this task, we classify the shocks according to the heliocentric distance at which they were observed by the space missions, from 0.29 to 0.99 au (Helios-A/B); near 1 au (Wind, ACE and STEREO-A/B); and from 1.35 to 5.4 au (Ulysses). We also differentiate the IP shocks into two populations, those with a detected ICME and those without it. In the same way, we also analyze the dependence of the distributions of the properties of the IP shocks with the solar activity cycle.
We find that there are no spacecraft biases positioned at 1 au, which is expected as there should be no differences for all shocks detected at the same distances from the Sun. As well as the distributions of shock parameters not present significant variations with the heliocentric distance. On the other hand, using the definition on the location angle lambda, the relative position between the spacecraft and the shock front of the structure (Janvier et al., 2014; 2015) we determine if there are a preferential orientation of the shocks/ICMEs, detected by different space missions, during several years.