The Brightness of Density Structures at Large Solar Elongation Angles: What is Being Observed by STEREO/SECCHI?

TL;DR

This paper examines how the complex 3-D structure of CMEs and observational geometry at large solar elongation angles affect brightness measurements by STEREO/SECCHI, emphasizing the importance of 3-D simulations for accurate interpretation.

Contribution

It demonstrates the necessity of 3-D magneto-hydrodynamic simulations to accurately interpret CME brightness features observed at large elongation angles.

Findings

Bright features are influenced by CME 3-D structure, solar rotation, and Thomson sphere geometry.

CME-driven shocks can be mistaken for other features without proper 3-D analysis.

Observed bright features may include dense streams compressed by shocks, not just CME fronts.

Abstract

We discuss features of coronal mass ejections (CMEs) that are specific to heliospheric observations at large elongation angles. Our analysis is focused on a series of two eruptions that occurred on 2007 January 24-25, which were tracked by the Heliospheric Imagers (HIs) onboard STEREO. Using a three-dimensional (3-D) magneto-hydrodynamic simulation of these ejections with the Space Weather Modeling Framework (SWMF), we illustrate how the combination of the 3-D nature of CMEs, solar rotation, and geometry associated with the Thomson sphere results in complex effects in the brightness observed by the HIs. Our results demonstrate that these effects make any in-depth analysis of CME observations without 3-D simulations challenging. In particular, the association of bright features seen by the HIs with fronts of CME-driven shocks is far from trivial. In this Letter, we argue that, on 2007 January 26, the HIs observed not only two CMEs, but also a dense corotating stream compressed by the CME-driven shocks.