Relative contribution of the magnetic field barrier and solar wind speed in ICME-associated Forbush decreases

TL;DR

This study analyzes 50 Forbush decreases linked to ICMEs, revealing that magnetic field and solar wind speed influence cosmic ray modulation, with solar wind speed playing a dominant role during recovery phases.

Contribution

It provides a detailed analysis of the relative effects of magnetic fields and solar wind speed on Forbush decreases, highlighting the dominant role of solar wind speed during recovery.

Findings

FD profiles are correlated with magnetic field and solar wind speed.

During recovery, FD is highly anti-correlated with solar wind speed.

FD duration is similar to solar wind speed profile duration, longer than magnetic field profile.

Abstract

We study 50 cosmic ray Forbush decreases (FDs) from the Oulu neutron monitor data during 1997-2005 that were associated with Earth-directed interplanetary coronal mass ejections (ICMEs). Such events are generally thought to arise due to the shielding of cosmic rays by a propagating diffusive barrier. The main processes at work are the diffusion of cosmic rays across the large-scale magnetic fields carried by the ICME and their advection by the solar wind. In an attempt to better understand the relative importance of these effects, we analyse the relationship between the FD profiles and those of the interplanetary magnetic field (B) and the solar wind speed (Vsw). Over the entire duration of a given FD, we find that the FD profile is generally well (anti)correlated with the B and Vsw profiles. This trend holds separately for the FD main and recovery phases too. For the recovery phases, however, the FD profile is highly anti-correlated with the Vsw profile, but not with the B profile. While the total duration of the FD profile is similar to that of the Vsw profile, it is significantly longer than that of the B profile.