  We present spatially-resolved X-ray observations of the binary T Tauri star
system V710 Tau. Using Chandra's Advanced CCD Imaging Spectrometer (ACIS), we
imaged this 3.2'' separation binary system, consisting of a classical T Tauri
star, V710 Tau N, and a weak-lined T Tauri star, V710 Tau S. The Chandra
ACIS-S3 images -- obtained in two 9 ks exposures separated by about three
months (2004 December and 2005 April) -- cleanly resolve the V710 Tau binary,
demonstrating that both stars emit X-rays and thereby enabling the first
spectral/temporal study of the individual components of this mixed (classical
and weak-lined) T Tauri star binary system. The northern component, V710 Tau N,
appears to have been in a flaring state during the first (2004 December)
exposure. During this flare event, the X-ray flux of the classical T Tauri star
hardened significantly. Single-component plasma models with plasma temperatures
in the range kT ~ 0.7-1.1 keV are adequate to fit the observed X-ray spectra of
V710 Tau S in 2004 December and both stars in 2005 April. The 2004 December
flare-state observation of V710 Tau N requires a higher-temperature plasma
component (kT ~ 2.5 - 3.0 keV) in addition to the soft component (kT ~ 0.5 keV)
and is better fit by a model that includes a slightly enhanced Ne/Fe abundance
ratio. These results are generally consistent with statistical contrasts
between the X-ray emission properties of classical (rapidly accreting) vs.
weak-lined (weakly accreting or non-accreting) T Tauri stars.
