6533b85bfe1ef96bd12bace7
RESEARCH PRODUCT
XMM-Newton spectroscopy of the metal depleted T Tauri star TWA 5
Beate StelzerGiovanni PeresAntonio MaggioCostanza ArgiroffiRalph Neuhäusersubject
PhysicsInfrared excessAstrophysics (astro-ph)FOS: Physical sciencesAstronomy and AstrophysicsAstrophysicsAstrophysicsCoronaSpectral lineAccretion (astrophysics)StarsT Tauri starSettore FIS/05 - Astronomia E AstrofisicaSpace and Planetary ScienceTW HydraeX-rays: stars techniques: spectroscopic stars: activity stars: abundances stars: pre-main sequence stars: individual: TWA 5Main sequencedescription
We present results of X-ray spectroscopy for TWA 5, a member of the young TW Hydrae association, observed with XMM-Newton. TWA~5 is a multiple system which shows Halpha emission, a signature typical of classical T Tauri stars, but no infrared excess. From the analysis of the RGS and EPIC spectra, we have derived the emission measure distribution vs. temperature of the X-ray emitting plasma, its abundances, and the electron density. The characteristic temperature and density of the plasma suggest a corona similar to that of weak-line T Tauri stars and active late-type main sequence stars. TWA 5 also shows a low iron abundance (~0.1 times the solar photospheric one) and a pattern of increasing abundances for elements with increasing first ionization potential reminiscent of the inverse FIP effect observed in highly active stars. The especially high ratio Ne/Fe~10 is similar to that of the classical T Tauri star TW Hya, where the accreting material has been held responsible for the X-ray emission. We discuss the possible role of an accretion process in this scenario. Since all T Tauri stars in the TW Hydrae association studied so far have very high Ne/Fe ratios, we also propose that environmental conditions may cause this effect.
| year | journal | country | edition | language |
|---|---|---|---|---|
| 2005-01-01 | Astronomy & Astrophysics |