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

被引：0

作者：

Argiroffi, C. ^{[1
]}

Maggio, A. ^{[2
]}

Peres, G. ^{[1
]}

机构：

[1] Dipartimento di Scienze Fisiche ed Astronomiche, Sezione di Astronomia, Università di Palermo, Piazza del Parlamente 1, 90134 Palermo, Italy

[2] INAF, Osservatorio Astronomico di Palermo, Piazza del Parlamente 1, 90134 Palermo, Italy

来源：

Astronomy and Astrophysics | 2007年 / 465卷 / 01期

关键词：

Aims. We study the properties of X-ray emitting plasma of MP Mus; an old classical T Tauri star. We check whether an accretion process could produce the observed X-ray emission and we derive 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 emitting plasma. Methods. XMM-Newton X-ray spectra allow us to measure plasma temperatures; abundances; and electron density. The density of cool plasma probes whether X-ray emission is produced by plasma heated in the accretion process. Results. 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 5 × 10-11 Mo yr -1. © ESO 2007;

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Journal article (JA)

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