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We present spatially-resolved X-ray observations of the binary T Tauri starsystem V710 Tau. Using Chandra's Advanced CCD Imaging Spectrometer (ACIS), weimaged this 3.2'' separation binary system, consisting of a classical T Tauristar, V710 Tau N, and a weak-lined T Tauri star, V710 Tau S. The ChandraACIS-S3 images -- obtained in two 9 ks exposures separated by about threemonths (2004 December and 2005 April) -- cleanly resolve the V710 Tau binary,demonstrating that both stars emit X-rays and thereby enabling the firstspectral/temporal study of the individual components of this mixed (classicaland 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 starhardened significantly. Single-component plasma models with plasma temperaturesin the range kT ~ 0.7-1.1 keV are adequate to fit the observed X-ray spectra ofV710 Tau S in 2004 December and both stars in 2005 April. The 2004 Decemberflare-state observation of V710 Tau N requires a higher-temperature plasmacomponent (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 abundanceratio. These results are generally consistent with statistical contrastsbetween the X-ray emission properties of classical (rapidly accreting) vs.weak-lined (weakly accreting or non-accreting) T Tauri stars.

Spatially-resolved Chandra Imaging Spectroscopy of the classical/weak-lined T Tauri system V710 Tau