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2002MNRAS.334..705S - Mon. Not. R. Astron. Soc., 334, 705-712 (2002/August-2)
Spherical cocoon models for the flat infrared spectrum of the T Tauri phenomenon.
SORRELL W.H.
Abstract (from CDS):
The static dust cocoon model is applied to the young T Tau binary system. The cocoon is illuminated by radiation emitted from the optical primary (T Tau N), which is a classical T Tauri star. The infrared secondary (T Tau S) is identified as a magnetic brown dwarf in binary orbital motion outside the cocoon, but still embedded in a large nebula of cold gas and dust distributed around the binary system. Both T Tau N and T Tau S are magnetically linked to each other. The radiative transfer model for the cocoon infrared energy distribution is compared with observational flux data for T Tau N. The model appears in good agreement with the data from the optical to submillimetre wavebands. The model shows an almost flat infrared spectrum for T Tau N, except for the strong 10-µm silicate band in emission as observed. It is suggested that the magnetic brown dwarf (T Tau S) undergoes episodic and luminous non-thermal infrared and radio outburst emissions. Such a possibility is well in accord with a non-thermal origin for the circular polarized radio emission observed from the T Tau system. Nevertheless, if future high-resolution observations prove that the blue continuum emission from T Tauri stars originates from stellar chromospheric activity or boundary-layer emission from an equatorial disc, then a spherical cocoon model for the T Tauri phenomenon is wrong.
Abstract Copyright: 2002 Blackwell Science Ltd
Journal keyword(s): radiative transfer - circumstellar matter - stars: individual: T Tau - stars: low-mass, brown dwarfs - stars: pre-main-sequence - infrared: stars
Simbad objects: 8
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