2008ApJ...683..893S

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 3 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_X∼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_X∼2.5-3.0 keV) in addition to the soft component (kT_X∼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) versus weak-lined (weakly accreting or nonaccreting) T Tauri stars.