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Theories of Heating of Solar and Stellar Chromospheres

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Solar Phenomena in Stars and Stellar Systems

Part of the book series: NATO Advanced Study Institutes Series ((ASIC,volume 68))

Abstract

In the outer atmosphere of stars a rise of the kinetic temperature to values above Teff is possible only if a large and persistent amount of mechanical heating is present. Constraints derived from empirical chromosphere models allow selection of important heating mechanisms from among a great number of possible processes. It appears that for non-magnetic regions short period acoustic waves and for magnetic regions Alfvén and slow mode magnetohydrodynamic waves are the dominant mechanisms. For non-magnetic cases new acoustic energy generation rates are reported. Non-magnetic theoretical chromosphere models for the sun and 10 other stars are discussed and compared with observations. Chromospheric heating in early type stars is briefly mentioned.

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© 1981 D. Reidel Publishing Company

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Ulmschneider, P. (1981). Theories of Heating of Solar and Stellar Chromospheres. In: Bonnet, R.M., Dupree, A.K. (eds) Solar Phenomena in Stars and Stellar Systems. NATO Advanced Study Institutes Series, vol 68. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-8479-0_13

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  • DOI: https://doi.org/10.1007/978-94-009-8479-0_13

  • Publisher Name: Springer, Dordrecht

  • Print ISBN: 978-94-009-8481-3

  • Online ISBN: 978-94-009-8479-0

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