Chandra X-ray Grating Observation Of The Weak-lined T Tau Binary HDE 245059

Details Chandra X-ray Grating Observation Of The Weak-lined T Tau Binary HDE 245059 Chandra X-ray Grating Observation Of The Weak-lined T Tau Binary HDE 245059

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...211.6223b&link_type=abstract

American Astronomical Society, AAS Meeting #211, #62.23; Bulletin of the American Astronomical Society, Vol. 39, p.851

Astronomy and Astrophysics

Astronomy

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Scientific paper

We present the Chandra High Energy Transmission Grating Spectrometer (HETGS) observation of HDE 245059. Our target is a young weak-lined T Tauri star (WTTS), member of the pre-main sequence group near Lambda Orionis (d 400 pc). HDE 245059 is among the brightest WTTS in the X-ray domain (log Lx 32 erg/s); previous ROSAT and ASCA observations showed a typical plasma temperature of 6 - 8 MK. Our high spatial resolution near-infrared observations with Keck indicate that HDE 245059 is in fact a binary separated by 0.87'', probably both components being WTTS based on their color indices. We detected both components of the binary in the zeroth order Chandra image and in the grating spectra. The lightcurves show X-ray variability of both sources and in particular a flaring event with a significant hardening of the hardness ratio in the weaker southern component. The spectra of both stars are similar; they show a combination of cool and hot plasma as demonstrated from the presence of several iron lines from Fe XVII to Fe XXV and a strong bremsstrahlung continuum at short wavelengths. We have extracted the combined zeroth order and grating spectra for the binary. We fitted them simultaneously in XSPEC with a 4-T collisional plasma in order to get the emission measure distribution and chemical abundances. The best-fit values for the temperatures are: 0.3, 0.7, 1.3 and 4.5 keV, with the dominant components at T = 0.7 and 1.3 keV. The abundance pattern show an inverse FIP effect, except for Ca which is at solar value.
M.Audard and C.Baldovin Saavedra acknowledge the support from Swiss National Science Fundation grant PP002-110504. M. Audard also received support from Chandra award SAO GO5-6012X.

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