Abstract
We have studied a sample of 51 nearby stars with estimated masses in the range 1.1 — 1.9 M⨀, to monitor the coronal and transition region emission level, during the evolutionary phases from the main sequence to the base of the red giant branch. The available data suggest a mass-dependent variation of the X-ray (0.16–4 keV) luminosity and the C IV (1550) line luminosity, linked to changes of the stellar internal structure, and rotational regime. We discuss a possible interpretation in terms of the changing efficiency of a stellar magnetic dynamo, and the relative importance of mechanical and magnetic heating of the stellar outer atmospheres.
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© 1993 Kluwer Academic Publishers
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Maggio, A., Sciortino, S., Bianchi, L., Harnden, F.R., Rosner, R. (1993). X-Ray and UV Emission from Post-Main-Sequence Stars: The Connection Between Surface Activity and Evolution. In: Linsky, J.F., Serio, S. (eds) Physics of Solar and Stellar Coronae: G.S. Vaiana Memorial Symposium. Astrophysics and Space Science Library, vol 183. Springer, Dordrecht. https://doi.org/10.1007/978-94-011-1964-1_34
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DOI: https://doi.org/10.1007/978-94-011-1964-1_34
Publisher Name: Springer, Dordrecht
Print ISBN: 978-0-7923-2346-4
Online ISBN: 978-94-011-1964-1
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