Non-conventional Approach for Deriving the Radial Sizes of Coronal Mass Ejections at Different Instances: Discrepancies in the Estimates Between Remote and In Situ Observations

TL;DR

This paper introduces a novel method to accurately determine the radial sizes and expansion speeds of CMEs at various stages, addressing discrepancies between remote sensing and in situ measurements to better understand CME evolution.

Contribution

The study presents a non-conventional approach combining 3D kinematic reconstructions and models to improve CME size and speed estimates during propagation from the Sun to Earth.

Findings

The new method yields more accurate CME size and speed estimates.

Significant discrepancies exist between remote and in situ observations.

Aspect ratio variations influence CME expansion behavior.

Abstract

Understanding the evolution of radial sizes and instantaneous expansion speeds of coronal mass ejections (CMEs) is crucial for assessing their impact duration on Earth's environment. We introduce a non-conventional approach to derive the CME's radial sizes and expansion speeds at different instances during its passage over a single-point in situ spacecraft. We also estimate the CME's radial sizes and expansion speeds during its journey from the Sun to 1 AU using the 3D kinematics of different CME features, including the leading edge (LE), center, and trailing edge (TE). The continuous 3D kinematics of the CME is estimated by employing the GCS and SSSE reconstruction methods on multi-point observations from coronagraphs and heliospheric imagers combined with the drag-based model. We choose the 2010 April 3 CME as a suitable case for our study, promising a more accurate comparison of its remote and in situ observations. We show that the introduced non-conventional approach can provide better accuracy in estimating radial sizes and instantaneous expansion speeds of CMEs at different instances. We examine the aspect ratio of the CME, which influences its expansion behavior and shows the discrepancy between its value in the corona and interplanetary medium. Our study highlights significant inconsistencies in the arrival time, radial size, and expansion speed estimates obtained from remote and in situ observations. We advocate for future studies leveraging multi-spacecraft in situ observations and our non-conventional approach to analyze them to improve the comprehension of CME dynamics in the solar wind.