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- W2134920662 abstract "Previous observations have shown that although correlations exist between chromospheric, transition region and coronal emission fluxes, the correlations between these fluxes and stellar rotational periods depend on the spectral type and luminosity class. The measured coronal temperatures (|$T_text c$|) also depend on the type of star, with clear distinctions between F and G/K dwarf stars and between dwarf and giant stars. Others have argued that these emission fluxes, or luminosities, normalized to the stellar bolometric values can be related more closely to the Rossby number, |$R_o$|. Assuming that the coronal gas energy density depends only on the magnetic energy density we derive a correlation between the parameters |$Em(T_text c)$| (the coronal emission measure), |$T_text c$|, |$(g_text *)$|, the surface gravity, and the required coronal magnetic field. This correlates well with the Rossby number for the dwarf stars. Separate scalings for |$Em(T_text c)$| and |$T_text c$| with |$g_text *$| and |$R_text O$| based on the ratio of conductive to radiative losses are examined and show that the products |$T_text cg^{1/2}_*$| and |$Em(T_text c)g^{1/2}_*$| scale with |$R_text O$|. We explore how evolved stars might be included by also considering correlations with the dynamo number. Coronal temperatures and emission measures therefore provide an empirical way of investigating convection zone properties." @default.
- W2134920662 created "2016-06-24" @default.
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- W2134920662 date "1991-09-01" @default.
- W2134920662 modified "2023-10-18" @default.
- W2134920662 title "The dependence of coronal temperatures on Rossby numbers" @default.
- W2134920662 cites W1617886986 @default.
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- W2134920662 doi "https://doi.org/10.1093/mnras/252.1.21p" @default.
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