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High Resolution X-ray Spectroscopy of the Post-T Tauri Star PZ Tel | | C. Argiroffi
; J.J. Drake
; A. Maggio
; G. Peres
; S. Sciortino
; F.R. Harnden
; | | Date: |
1 Mar 2004 | | Journal: | Astrophys.J. 609 (2004) 925-934 | | Subject: | astro-ph | | Affiliation: | Dipartimento di Scienze Fisiche ed Astronomiche, Sezione di Astronomia, Università di Palermo, Italy, Smithsonian Astrophysics Observatory, Cambridge, MA, INAF - Osservatorio Astronomico di Palermo, Italy | | Abstract: | We present an analysis of the Chandra High Energy Transmission Grating Spectrometer observation of the rapidly rotating P_(rot)=0.94 d post T Tauri (~20 Myr old) star PZ Telescopii, in the Tucana association. Using two different methods we have derived the coronal emission measure distribution, em(T), and chemical abundances. The em(T) peaks at log T = 6.9 and exhibits a significant emission measure at temperatures log T > 7. The coronal abundances are generally ~0.5 times the solar photospheric values that are presumed fairly representative of the composition of the underlying star. A minimum in abundance is seen at a first ionization potential (FIP) of 7-8 eV, with evidence for higher abundances at both lower and higher FIP, similar to patterns seen in other active stars. From an analysis of the He-like triplet of Mg XI we have estimated electron densities of ~10^(12)-10^(13) cm^(-3). All the coronal properties found for PZ Tel are much more similar to those of AB Dor, which is slightly older than PZ Tel, than to those of the younger T Tauri star TW Hya. These results support earlier conclusions that the soft X-ray emission of TW Hya is likely dominated by accretion activity rather than by a magnetically-heated corona. Our results also suggest that the coronae of pre-main sequence stars rapidly become similar to those of older active main-sequence stars soon after the accretion stage has ended. | | Source: | arXiv, astro-ph/0403017 | | Services: | Forum | Review | PDF | Favorites | |
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