Astronomy and Astrophysics – Astronomy
Scientific paper
Jun 1988
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988esasp.281a.327l&link_type=abstract
In ESA, A Decade of UV Astronomy with the IUE Satellite, Volume 1 p 327-330 (SEE N89-10682 01-89)
Astronomy and Astrophysics
Astronomy
Carbon Stars, Chromosphere, Iue, Line Spectra, Spaceborne Astronomy, Ultraviolet Astronomy, Ultraviolet Spectra, Atmospheric Models, Stellar Models, Stellar Temperature
Scientific paper
Based on adopted photospheric plus chromospheric models, synthetic fluxes of the C II (UV 0.01) and fluxes and profiles for the Mg II (UV 1) lines in complete (CRD) and partial (PRD) redistribution are generated and compared to IUE spectra of the carbon star TX Psc. Non-LTE calculations with the program PANDORA are made for H, C, Na, Mg, and Ca. For CRD and a well constrained chromospheric model, the best fit to the Mg II line profiles gives a flux in the C II lines (produced at the same depth as the Mg II lines) 2.6 times too great and produces too much emission in the Mg II line wings. The PRD in the Mg II h and k lines in an expanding chromosphere with an adjusted temperature structure produces the observed Mg II emission. The reduction in temperature produces C II fluxes that matches the IUE low resolution spectra.
Avrett Eugene H.
Johnson Hollis R.
Luttermoser Donald G.
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