2014/07/31 by P. Pagano, Paolo Pagano, D. H. Mackay +2
Physics and Astronomy · #Astrobiology #Astronomy #Astrophysics #Computer science #Corona (planetary geology) #Coronal mass ejection #Extreme ultraviolet #Flux (metallurgy) #Flux tube #Ionosphere and magnetosphere dynamics #Magnetic field #Magnetic flux #Materials science #Optics #Physics #Plasma #Radiative cooling #Rope #Solar and Space Plasma Dynamics #Solar wind #Stellar, planetary, and galactic studies #astro-ph.SR
paper · pdf · doi:10.1051/0004-6361/201424019
published as A&A 568, A120 (2014)
arxiv created 2014/07/31 · openalex publication_date 2014/07/31 · arxiv updated 2014/09/05 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/06
Context. Coronal mass ejections (CMEs) are the most violent phenomena observed on the Sun. Currently, extreme ultraviolet (EUV) images from the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamic Observatory (SDO) are providing new insights into the early phase of CME evolution. In particular, observations now show the ejection of magnetic flux ropes from the solar corona and how they evolve into CMEs. While this is the case, these observations are difficult to interpret in terms of basic physical mechanisms and quantities. To fully understand CMEs we need to compare equivalent quantities derived from both observations and theoretical models. This will aid in bridging the gap between observations and models.