  The atmospheric structure of T Tauri Stars (TTSs) and its connection with the
large scale outflow is poorly known. Neither the effect of the magnetically
mediated inter- action between the star and the disc in the stellar atmosphere
is well understood. The Mg II multiplet is a fundamental tracer of TTSs
atmospheres and outflows, and is the strongest feature in the near-ultraviolet
spectrum of TTSs. The International Ultraviolet Explorer and Hubble Space
Telescope data archives provide a unique set to study the main physical
compounds contributing to the line profile and to derive the properties of the
line formation region. The Mg II profiles of 44 TTSs with resolution 13,000 to
30,000 are available in these archives. In this work, we use this data set to
measure the main observables: flux, broadening, asymmetry, terminal velocity of
the outflow, and the velocity of the Discrete Absorption Components. For some
few sources repeated observations are available and variability has been
studied. There is a warm wind that at sub-AU scales absorbs the blue wing of
the Mg II profiles. The main result found in this work is the correlation
between the line broadening, Mg II flux, terminal velocity of the flow and
accretion rate. Both outflow and magnetospheric plasma contribute to the Mg II
flux. The flux-flux correlation between Mg II and C IV or He II is confirmed;
however, no correlation is found between the Mg II flux and the ultraviolet
continuum or the H2 emission.
