The energy input mechanism into the lower transition regions between stellar chromospheres and coronae

Details The energy input mechanism into the lower transition regions between stellar chromospheres and coronae The energy input mechanism into the lower transition regions between stellar chromospheres and coronae

Jun 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988esasp.281a.315b&link_type=abstract

In ESA, A Decade of UV Astronomy with the IUE Satellite, Volume 1 p 315-317 (SEE N89-10682 01-89)

Astronomy and Astrophysics

Astronomy

Chromosphere, Energy Transfer, Iue, Spaceborne Astronomy, Stellar Coronas, Ultraviolet Astronomy, Ultraviolet Spectra, Stellar Temperature, T Tauri Stars, Temperature Gradients

Scientific paper

The ratio of the emission line fluxes for the C II and C IV lines in the lower transition regions (T = 30,000 to 100,000 K) between stellar chromospheres and transition layers is shown to depend mainly on the temperature gradient in the line emitting regions which can therefore be determined from this line ratio. From the observed constant (within the limits of observational error) ratio of the emission line fluxes of the C II (1335 A) and C IV (1550 A) lines it is concluded that the temperature gradients in the lower transition layers are similar for the large majority of stars independently of Teff, L, and degree of activity. This means that the temperature dependence of the damping length for the mechanical flux must be the same for all these stars. Since for different kinds of mechanical fluxes the dependence of the damping length on gas pressure and temperature is quite different, it is concluded that the same heating mechanism must be responsible for the heating of all the lower transition layers of these stars, regardless of their chromospheric activity. Only the amount of mechanical flux changes. The T Tauri stars are exceptions: their emission lines are probably mainly due to circumstellar material.

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