Astronomy and Astrophysics – Astronomy
Scientific paper
May 1991
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991mnras.250...14t&link_type=abstract
Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 250, May 1, 1991, p. 14-23.
Astronomy and Astrophysics
Astronomy
28
Chromosphere, Dwarf Stars, K Stars, Late Stars, Stellar Models, Stellar Spectra, Fine Structure, Infrared Spectra, Nonequilibrium Thermodynamics, Photosphere, Stellar Atmospheres, Stellar Temperature, Visible Spectrum
Scientific paper
A new model of the lower chromosphere of the dwarf K2 star Epsilon Eridani is derived by matching flux profiles of the Ca IR triplet lines 8498 and 8542 A H-alpha and H-beta lines and the Na D lines (all observed simultaneously at the AAT), and the Ca II K line. The coupled non-LTE equations of statistical equilibrium and radiative transfer are solved under the constraint of hydrostatic equilibrium using the Carlsson (1986) code. Within the framework of the model, the Na D lines are an important photospheric diagnostic, and the Ca IR triplet lines can be used to locate the temperature minimum. The computed H-alpha and H-beta depths are highly sensitive constraints on the transition zone gradients and base pressures allowing us to derive a pressure at the base of the transition zone of 0.9 dyn/cm.
Rees David E.
Robinson Richard D.
Thatcher John D.
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