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Einstein Observatory coronal temperatures of late-type stars
Schmitt, J. H. M. M.; Collura, A.; Sciortino, S.; Vaiana, G. S.; Harnden, F. R., Jr.; Rosner, R.
AA(Max-Planck-Institut für Physik und Astrophysik, Garching bei München, Germany), AB(CNR, Istituto per le Applicazioni Interdisciplinari della Fisica, Palermo, Italy), AC(Palermo, Osservatorio Astronomico, Italy), AD(Palermo, Osservatorio Astronomico, Italy), AE(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA)
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 365, Dec. 20, 1990, p. 704-728. Research supported by the Max-Planck-Gesellschaft, CNR, and ASI. (ApJ Homepage)
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NASA/STI Keywords:
Heao 2, Late Stars, Stellar Coronas, Stellar Spectra, Stellar Temperature, X Ray Sources, Proportional Counters, Spectrum Analysis, Stellar Models, X Ray Spectra
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The results are presented of a survey of the coronal temperatures of late-type stars using the Einstein Observatory IPC. The spectral analysis shows that the frequently found one- and two-temperature descriptions are mainly influenced by the SNR of the data and that models using continuous emission measure distributions can provide equally adequate and physically more meaningful and more plausible descriptions. Intrinsic differences in differential emission measure distributions are found for four groups of stars. M dwarfs generally show evidence for high-temperature gas in conjunction with lower-temperature material, while main-sequence stars of types F and G have the high-temperature component either absent or very weak. Very hot coronae without the lower-temperature component appearing in dwarf stars are evident in most of the giant stars studied. RS CVn systems show evidence for extremely hot coronae, sometimes with no accompanying lower-temperature material.

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