Abstract
Many objects which emit X-rays are also sources of uv emission from plasmas at temperatures between 104 and 2 × 105 K. To obtain a full understanding of, for example, stellar coronae, simultaneous studies in the uv, far uv and X-ray regions are ideally required. The present review summarises the methods by which uv spectra can be analysed to give plasma conditions such as the density and outlines how the uv spectra can be used to investigate the physical processes controlling energy balance in chromospheres and coronae.
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© 1988 Kluwer Academic Publishers
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Jordan, C. (1988). Ultraviolet Stellar Spectroscopy. In: Pallavicini, R. (eds) Hot Thin Plasmas in Astrophysics. NATO ASI Series, vol 249. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-3065-0_6
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DOI: https://doi.org/10.1007/978-94-009-3065-0_6
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