2015/10/01 by A. A. Reva, Anton Reva, Sergey Shestov +6 · 23 citations
Biochemistry, Genetics and Molecular Biology · Mathematics · Physics and Astronomy · #Approx #Atomic physics #Combinatorics #Computer science #Excited state #Geomagnetism and Paleomagnetism Studies #Geometry #Ionosphere and magnetosphere dynamics #Line (geometry) #Loop (graph theory) #Mathematics #Monochromatic color #Optics #Physics #Solar and Space Plasma Dynamics #astro-ph.SR
paper · pdf · doi:10.1007/s11207-015-0769-x
published in Solar Physics 290(10), 2909-2921 (Springer Science+Business Media) · Published in Solar Physics, 2015. Online first
openalex publication_date 2015/10/01 · arxiv created 2015/10/08 · arxiv updated 2015/11/20 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We present observations of hot arcades made with the Mg XII spectroheliograph onboard the CORONAS-F mission, which provides monochromatic images of hot plasma in the Mg XII 8.42 A resonance line. The arcades were observed to form above the polarity inversion line between Active Regions NOAA 09847 and 09848 at four successive episodes: at 09:18, 14:13, and 22:28 UT on 28 February 2002, and at 00:40 UT on 1 March 2002. The arcades all evolved in the same way: a) a small flare (precursor) appeared near the edge of the still invisible arcade, b) the arcade brightened in a wave-like manner - closer loops brightened earlier, and c) the arcade intensity gradually decreased in ≈ 1 h. The estimated wave speed was ≈ 700 km s-1, and the distance between the hot loops was ≈ 50 Mm. The arcades formed without visible changes in their magnetic structure. The arcades were probably heated up by the instabilities of the current sheet above the arcade, which were caused by an MHD wave excited by the precursor.