ROSAT X-Ray Spectral Properties of Nearby Young Associations: TW Hydrae, Tucana-Horologium, and the β Pictoris Moving Group
© 2003 The American Astronomical Society.
We acknowledge incisive comments from the referee and Inseok Song that substantially improved this paper. Ms. Rich acknowledges support from a summer internship program funded by the Industrial Associates of the Center for Imaging Science at RIT.ISSN:1538-4365 Note: imported from RIT’s Digital Media Library running on DSpace to RIT Scholar Works in February 2014.
We present archival ROSAT data for three recently identified, nearby (D < 70 pc), young (~10−40 Myr) stellar associations: the TW Hydrae Association, the Tucana-Horologium Association, and the beta Pic Moving Group. The distributions of ROSAT X-ray hardness ratios (HR1, HR2) for these three groups, whose membership is dominated by low-mass, weak-lined T Tauri stars, are tightly clustered and very similar to one another. The value of HR1 for TW Hya itself — the only bona fide classical T Tauri star in any of the nearby groups — is clearly anomalous among these nearby young stars. We compare the hardness ratio distributions of stars in the three nearby groups with those of T Tauri stars, the Hyades, and main sequence dwarfs in the field. This comparison demonstrates that the X-ray spectra of F through M stars soften with age, and that F and G stars evolve more rapidly in X-ray spectral hardness than do K and M stars. It is as yet unclear whether this trend can be attributed to age-dependent changes in the intrinsic X-ray spectra of stars of type F and later, to a decrease in the column density of circumstellar gas (e.g., in residual protoplanetary disks), or to the diminishing contributions of star-disk interactions to X-ray emission. Regardless, these results demonstrate that analysis of archival ROSAT X-ray spectral data can help both to identify nearby, young associations and to ascertain the X-ray emission properties of members of known associations (Refer to PDF file for exact formulas).