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Published in

Hans Publishers, Astronomy & Astrophysics, 1(465), p. L5-L8

DOI: 10.1051/0004-6361:20067016

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X-ray emission from MP Muscae: an old classical T Tauri star

Journal article published in 2007 by Costanza Argiroffi, A. Maggio ORCID, Giovanni Peres
This paper is made freely available by the publisher.
This paper is made freely available by the publisher.

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Data provided by SHERPA/RoMEO

Abstract

We study the properties of X-ray emitting plasma of MP Mus, an old classical T Tauri star. We aim at checking whether an accretion process produces the observed X-ray emission and at deriving the accretion parameters and the characteristics of the shock-heated plasma. We compare the properties of MP Mus with those of younger classical T Tauri stars to test whether age is related to the properties of the X-ray emission plasma. XMM-Newton X-ray spectra allows us to measure plasma temperatures, abundances, and electron density. In particular the density of cool plasma probes whether X-ray emission is produced by plasma heated in the accretion process. X-ray emission from MP Mus originates from high density cool plasma but a hot flaring component is also present, suggesting that both coronal magnetic activity and accretion contribute to the observed X-ray emission. We find a Ne/O ratio similar to that observed in the much younger classical T Tauri star BP Tau. From the soft part of the X-ray emission, mostly produced by plasma heated in the accretion shock, we derive a mass accretion rate of 5x10^{-11} M_{sun} yr^{-1}. Comment: 4 pages, 4 postscript figures, accepted for publication as a Letter in Astronomy and Astrophysics