2003/11/16 by J. Sanz-Forcada, F. Favata, G. Micela · 1 citation
Physics and Astronomy · #Abundance (ecology) #Astronomy and Astrophysical Research #Coronal hole #Coronal loop #Coronal plane #Flux (metallurgy) #Line (geometry) #Solar and Space Plasma Dynamics #Stars #Stellar atmosphere #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1051/0004-6361:20034466
published as Astron.Astrophys. 416 (2004) 281-290 · 10 pages, Online material: 8 pages (online material is included in the file). Accepted by A&A
arxiv created 2003/11/16 · openalex publication_date 2004/02/23 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We report a detailed analysis of the coronal abundance of 4 stars with varying levels of activity and with accurately known photospheric abundances. The coronal abundance is determined here using a line flux analysis and a full determination of the differential emission measure. Photospheric abundance values are taken from the literature. Previous coronal abundance determinations have generally been compared to solar photospheric abundances; from this a number of general properties have been inferred, such as the presence of a coronal metal depletion with an inverse First Ionization Potential correlated with activity level. Here we show that, when coronal abundances are compared with real photospheric values for the individual stars, the resulting pattern can be very different. Also, we present evidence that, in some cases, the coronal metal abundance may not be uniform in the corona; in particular it can vary with the temperature of the emitting plasma.