Revealing the properties of the weak-lined TTauri binary HDE 245059 with Chandra HETGS and Keck

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We present the Chandra (HETGS) and Keck observations of the young weak-lined T Tauri star HDE 245059 located in the Lambda-Ori star forming region. Our observations in both wavelength regimes have shown that the star is in fact a binary separated by 0.87 arcsec. In the X-rays the plasma properties of both binary components are similar; they show a wide range of plasma temperatures from about 6 to 40 MK dominated by plasma between 8 to 15 MK. The hydrogen column density is low (NH ~ 8x10^19 cm-2), probably due to the clearing of the region by a supernova explosion 1 Myr ago. The coronal abundances show an inverse FIP effect, which is also observed in other young active stars. We have obtained line fluxes from the He-like triplets finding no evidence of high density plasma, which is consistent with the absence of accretion in the WTT binary. Furthermore, using the near-infrared photometry and evolutionary models we have also obtained the first estimates for the masses, effective temperatures, and radii for the binary components. According to our study HDE 245059 is 2-3 Myr old, accounting on our estimates the binary has experienced the supernova explosion leaving unchanged its coronal properties.

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