A multi-spacecraft view of a giant filament eruption during 26/27 September 2009

TL;DR

This study uses multi-spacecraft observations and a new tomographic method to analyze the 3D evolution and kinematics of a giant filament eruption in 2009, providing insights into its propagation and acceleration.

Contribution

It introduces a novel tomographic reconstruction technique for 3D filament analysis and applies it to multi-view data to better understand eruption dynamics.

Findings

Exponential rise profile fits filament acceleration better than other functions.

The filament's true propagation direction was estimated using combined observations.

The new tomographic method enhances 3D reconstruction accuracy.

Abstract

We analyze multi-spacecraft observations of a giant filament eruption that occurred during 26 and 27 September 2009. The filament eruption was associated with a relatively slow coronal mass ejection (CME). The filament consisted of a large and a small part, both parts erupted nearly simultaneously. Here we focus on the eruption associated with the larger part of the filament. The STEREO satellites were separated by about 117 degree during this event, so we additionally used SoHO/EIT and CORONAS/TESIS observations as a third eye (Earth view) to aid our measurements. We measure the plane-of-sky trajectory of the filament as seen from STEREO-A and TESIS view-points. Using a simple trigonometric relation, we then use these measurements to estimate the true direction of propagation of the filament which allows us to derive the true R=R_sun v/s time profile of the filament apex. Furthermore, we develop a new tomographic method that can potentially provide a more robust three-dimensional reconstruction by exploiting multiple simultaneous views. We apply this method also to investigate the 3D evolution of the top part of filament. We expect this method to be useful when SDO and STEREO observations are combined. We then analyze the kinematics of the eruptive filament during its rapid acceleration phase by fitting different functional forms to the height-time data derived from the two methods. We find that, for both methods, an exponential function fits the rise profile of the filament slightly better than parabolic or cubic functions. Finally, we confront these results with the predictions of theoretical eruption models.