On the spectral form of the infrared excess component in T Tauri systems

Details On the spectral form of the infrared excess component in T Tauri systems On the spectral form of the infrared excess component in T Tauri systems

Feb 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987pasp...99..141r&link_type=abstract

Astronomical Society of the Pacific, Publications (ISSN 0004-6280), vol. 99, Feb. 1987, p. 141-145.

Astronomy and Astrophysics

Astronomy

50

B Stars, Infrared Spectra, Stellar Radiation, Stellar Spectra, T Tauri Stars, Broadband, Disks, Least Squares Method, Spectral Energy Distribution

Scientific paper

The spectral form of the IR-excess component is derived for a sample of eight well-observed T Tauri stars and one Herbig Be star. The fundamental assumption is that the photospheric contribution at IR wavelengths can be estimated by fitting an appropriate photosphere at the I filter, after correction for interstellar reddening. The authors find that the IR-excess components obtained in this way are remarkably similar from star to star, suggesting a common form for T Tauri IR excesses at wavelengths shortward of 20 μm. The observed slope for the spectral energy distribution of the IR excess is not quite as negative as that expected from Keplerian accretion disks and from disks which simply reprocess stellar light. The fraction of the system luminosity attributed to thermal dust emission ranges from about 0.4 to almost 0.8 in the sample. These fractional IR excesses are too large to be explained solely by reprocessing of stellar light in a thin disk, and suggest the presence of some intrinsic disk luminosity.

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