Abstract
We have observed the T Tau multiple star system using the Multielement Radio-linked Interferometer Network at a frequency of 5 GHz. The compact centimeter wavelength radio emission from T Tau S has been found to consist of at least two components separated by approximately 70 mas in right ascension at Julian epoch 2001.89. Using this data and that previously published, we show that the most intense, compact radio emission may not all be coincident in position but associated with the M-type star in the binary system T Tau S. This emission may be due to magnetic reconnection processes in the YSO system. The estimated masses of the stars using the Hipparcos parallax are 4.0 M☉ for Sa and 1.0 M☉ for Sb. However, using the currently accepted parallax for the Taurus-Auriga complex of 140 pc, the value of these masses is reduced by a factor of 2. This is consistent with T Tau Sa being a pre-main-sequence star.
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