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The chromospheric hypothesis for the T Tauri phenomenon
Calvet, N.; Basri, G.; Kuhi, L. V.
AA(California, University, Berkeley, CA; Centro de Investigaciones de Astronomia, Merida, Venezuela), AB(California, University, Berkeley, CA), AC(California, University, Berkeley, CA)
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 277, Feb. 15, 1984, p. 725-737. Research supported by the Alexander von Humboldt Stiftung. (ApJ Homepage)
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NASA/STI Keywords:
Chromosphere, Late Stars, Stellar Evolution, Stellar Models, T Tauri Stars, Absorption Spectra, Abundance, Emission Spectra, Line Spectra, Main Sequence Stars, Spectral Energy Distribution, Stellar Atmospheres, Stellar Temperature, Ultraviolet Spectra
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A number of model atmospheres for T Tauri stars are constructed which are characterized by a late-type photosphere plus a chromosphere with a deep-lying temperature minimum. Parameter studies of these models show that they reproduce reasonably well the Ca II, Mg II emission-line fluxes, the continuous energy distribution, the absorption lines, and the ultraviolet lines. The presence of a chromosphere also likely accounts for the veiling phenomenon but is not sufficient to produce the large observed H alpha fluxes in many T Tauri stars, which require a much larger extended emitting region. However, it seems adequate to account for many spectral features of the average T Tauri star which are qualitatively similar to a normal active late-type star.

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