2010/01/12 by S. W. McIntosh, Scott W. McIntosh, Bart De Pontieu +3
Physics and Astronomy · #Astro and Planetary Science #Astronomy #Astrophysics #Coronal mass ejection #Extreme ultraviolet #Extreme ultraviolet lithography #Heliosphere #Magnetic field #Meteorology #Optics #Outflow #Physics #Solar and Space Plasma Dynamics #Solar wind #Spacecraft #Stellar, planetary, and galactic studies #astro-ph.SR
paper · pdf · doi:10.1007/s11207-010-9538-z
published as Solar Physics, 2010, Volume 265, Issue 1-2, pp. 5-17 · Accepted to appear in Solar Physics Topical Issue titled "Remote Sensing of the Inner Heliosphere". Manuscript has 14 pages, 5 color figures. Movies supporting the figures can be found in http://download.hao.ucar.edu/pub/mscott/papers/Weather
arxiv created 2010/01/12 · openalex publication_date 2010/03/22 · arxiv updated 2010/08/31 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We present the application of novel diagnostics to the spectroscopic observation of a Coronal Mass Ejection (CME) on disk by the Extreme Ultraviolet Imaging Spectrometer (EIS) on the Hinode spacecraft. We apply a recently developed line profile asymmetry analysis to the spectroscopic observation of NOAA AR 10930 on 14 – 15 December 2006 to three raster observations before and during the eruption of a 1000 km s −1 halo CME. We see the impact that the observer’s line-of-sight and magnetic field geometry have on the diagnostics used. Further, and more importantly, we identify the on-disk signature of a high-speed outflow behind the CME in the dimming region arising as a result of the eruption. Supported by recent coronal observations of the STEREO spacecraft, we speculate about the momentum flux resulting from this outflow as a secondary momentum source to the CME. The results presented highlight the importance of spectroscopic measurements in relation to CME kinematics, and the need for full-disk synoptic spectroscopic observations of the coronal and chromospheric plasmas to capture the signature of such explosive energy release as a way of providing better constraints of CME propagation times to L1, or any other point of interest in the heliosphere.