The importance of surface inhomogeneities for K and M dwarf chromospheric fluxes

Details The importance of surface inhomogeneities for K and M dwarf chromospheric fluxes The importance of surface inhomogeneities for K and M dwarf chromospheric fluxes

Aug 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993a%26as..100..343p&link_type=abstract

Astronomy and Astrophysics Supplement Series (ISSN 0365-0138), vol. 100, no. 2, p. 343-369.

Astronomy and Astrophysics

Astrophysics

41

Chromosphere, Dwarf Stars, K Stars, Late Stars, M Stars, Stellar Atmospheres, Stellar Luminosity, Balmer Series, Inhomogeneity, Spectrophotometry

Scientific paper

We present published and archived spectroscopic and spectrophotometric data of H-alpha, Ca II, Mg II, and X-rays for a large sample of K and M dwarfs. The data set points to the importance that surface inhomogeneities have in the flux luminosity diagrams in these late-type dwarfs, irrespective of whether the Balmer lines are in emission or absorption. Although supporting the fact that cooler stars exhibit increasing levels of surface activity, evident through an increasing incidence of Balmer emission, surface inhomogeneities, or variations in the local temperature and density structure, at the chromospheric level, dominate the total Ca II and Mg II fluxes. We show that the flux-flux and luminosity-luminosity relations indicate differing extents of inhomogeneity from the chromosphere through to the corona. A good correlation between Ca II and Mg II fluxes indicates that they are formed in overlapping regions of the chromosphere, so that the contribution of surface inhomogeneities is not evident from this particular flux-flux diagram. In the region of the upper chromosphere through to the transition and corona, the correlation between Ly-alpha and X-ray fluxes indicates regions with similar levels of areal inhomogeneity. This appears to be uncorrelated with that at the chromospheric level.

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