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X-ray astronomy of stellar coronae
Open accessAbstract
Abstract.X-ray emission from stars in the cool half of the Hertzsprung-Russell diagram is generally attributed to the presence of a magnetic corona that contains plasma at temperatures exceeding 1 million K. Coronae are ubiquitous among these stars, yet many fundamental mechanisms operating in their magnetic fields still elude an interpretation through a detailed physical description. Stellar X-ray astronomy is therefore contributing toward a deeper understanding of the generation of magnetic fields in magnetohydrodynamic dynamos, the release of energy in tenuous astrophysical plasmas through various plasma-physical processes, and the interactions of high-energy radiation with the stellar environment. Stellar X-ray emission also provides important diagnostics to study the structure and evolution of stellar magnetic fields from the first days of a protostellar life to the latest stages of stellar evolution among giants and supergiants. The discipline of stellar coronal X-ray astronomy has now reached a level of sophistication that makes tests of advanced theories in stellar physics possible. This development is based on the rapidly advancing instrumental possibilities that today allow us to obtain images with sub-arcsecond resolution and spectra with resolving powers exceeding 1000. High-resolution X-ray spectroscopy has, in fact, opened new windows into astrophysical sources, and has played a fundamental role in coronal research.The present article reviews the development and current status of various topics in the X-ray astronomy of stellar coronae, focusing on observational results and on theoretical aspects relevant to our understanding of coronal magnetic structure and evolution.
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Citations
Cited by
The Chemical Composition of the Sun
Asplund, M., Grevesse, N., Sauval, A. J., & Scott, P. (2009) · Annual Review of Astronomy and Astrophysics · doi:10.1146/annurev.astro.46.060407.145222 · Cited by 9,346
“Their sample is, however, heavily biased towards active stars, which experience an inverse FIP effect: elements with χion > 10 eV are enhanced in the corona compared with low ionization potential species (Güdel 2004).”
BackgroundAn intermediate-mass black hole of over 500 solar masses in the galaxy ESO 243-49
Farrell, S. A., Webb, N. A., Barret, D., Godet, O., & Rodrigues, J. M. (2009) · Nature · doi:10.1038/nature08083 · Cited by 508
Wood, B. E., & Linsky, J. L. (2010) · The Astrophysical Journal · doi:10.1088/0004-637x/717/2/1279 · Cited by 262
THE EVOLUTION OF STELLAR ROTATION AND THE HYDROGEN ATMOSPHERES OF HABITABLE-ZONE TERRESTRIAL PLANETS
Johnstone, C. P., Güdel, M., Stökl, A., Lammer, H., Tu, L., Kislyakova, K. G., Lüftinger, T., Odert, P., Erkaev, N. V., & Dorfi, E. A. (2015) · The Astrophysical Journal · doi:10.1088/2041-8205/815/1/l12 · Cited by 151
Self-citationHydrodynamic escape of water vapor atmospheres near very active stars
Johnstone, C. P. (2020) · The Astrophysical Journal · doi:10.3847/1538-4357/ab6224 · Cited by 63
Metadata
- Authors
- G�del, M.
- Venue
- The Astronomy and Astrophysics Review
- Published
- 2004-09
- Volume
- 12
- Issue
- 2-3
- ISSN
- 0935-4956 (ISSN-L)
- 1432-0754
- OpenAlex
- W2138534553
- Cited by
- 413
- References
- 0
- FWCI
- 12.60
- Type
- journal article
- Language
- en
- Open access
- green
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