engleski

Probing CME evolution using galactic cosmic ray measurements

One of the most common in situ signatures of CMEs are short-term reductions in Galactic cosmic ray (GCR) flux (i.e., Forbush decreases) measured by ground-based instruments on Earth and Mars, and by various spacecraft in the heliosphere (most recently by Solar Orbiter). We have recently developed an analytical model to explain CME-related Forbush decreases using an expansion-diffusion approach (ForbMod, Dumbovic et al., 2018 ; 2020). According to the model, the amplitude of the depression at a given point in the heliosphere depends on the initial CME properties as well as its evolutionary properties. By constraining the initial CME properties using remote observations and the final state properties using insitu measurements, we can apply reverse modelling to gain insight into CME evolution. We test the applicability by comparing model and observations using SOHO/LASCO and STEREO/SECCHI remote observations of the Sun, near-Earth in situ plasma and magnetic field measurements from OMNI, and GCR measurements from SOHO/EPHIN.

Sun, Heliosphere, coronal mass ejection, forbush decreases, galactic cosmic rays

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