Astronomy and Astrophysics – Astronomy
Scientific paper
Jan 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...281..471m&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 281, no. 2, p. 471-485
Astronomy and Astrophysics
Astronomy
5
Stellar Models, Stellar Spectra, Stellar Winds, Stochastic Processes, T Tauri Stars, Ultraviolet Astronomy, Ultraviolet Spectra, Visible Spectrum, Astronomical Spectroscopy, Atmospheric Models, Balmer Series, Emission Spectra, Mathematical Models, Stellar Atmospheres, Stellar Luminosity, Stellar Mass
Scientific paper
T Tauri stars show non-photospheric excess emission at ultraviolet and optical wavelengths. The interpretation of this excess is usually done in terms of the deep chromosphere or boundary layer model. In this paper we show that the emission of stochastic stellar winds could contribute significantly to the formation of the excess emission blue ward of 1 micron. Stochastic stellar winds have already been discussed by Mitskevich et al. (1993) and proved able to reproduce the observed line profiles. We show here that, with the same parameters, they are also able to fit the amount of the ultraviolet and visual excess, its spectral slope and the luminosities of the Balmer lines. The slope of the optical/UV excess depends mainly on gas density. According to our modeling it is formed by a gas with density 1013 - 1014/cc and can be easily explained by chromosphere, boundary layer, or stochastic wind model. Therefore, the slope of the excess by itself cannot discriminate between the above models. Free-free emission from stochastic winds cannot account for the observed infrared excess. The possible role of dust will be discussed in a following paper.
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