Reconciling Extreme-Ultraviolet and Radio Observations of the Sun’s Corona

摘要: The Sun's corona, which is composed of plasma at a temperature few millions degrees, can be best viewed in two electromagnetic domains, one from wavelengths angstroms to hundreds (in the soft X-ray and EUV domain), other centimeters several tens radio domain). In this paper, we present quantitative comparison coronal observations made these domains with high spatial resolution over full disk Sun. were taken EIT (Extreme-Ultraviolet Imaging Telescope) on board SOHO (Solar Heliospheric Observatory), VLA (Very Large Array). sets images show very similar morphologies, indicating that different originate common solar features. We predict fluxes using emission measure corona calculated observations, adopting Meyer's table abundances for calculations. each seven investigated, there always exists good linear correlation pixel-by-pixel plot between predicted observed flux features wide range variation. Nevertheless, systematically larger than by factor 2.0 ± 0.2, average. attribute difference underestimation abundance Fe relative H adopted Meyer. On basis, place absolute 7.8 × 10-5, has an enrichment 2.4 accepted photospheric abundance.