X-rays from the Most Active T Tauri Stars: Accretion Shocks or Magnetic Heating?

Details X-rays from the Most Active T Tauri Stars: Accretion Shocks or Magnetic Heating? X-rays from the Most Active T Tauri Stars: Accretion Shocks or Magnetic Heating?

Oct 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005xmm..prop..135w&link_type=abstract

XMM-Newton Proposal ID #04034601

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Stars, White Dwarfs, Solar System, S Cra, Xmm-Newton Proposal 04034601

Scientific paper

What is the nature of the X-ray emission observed in the extreme T~Tauri stars? Does it arise in a heavily absorbed but otherwise solar-like corona, in a thin dense plasma arising from the accretion shock, or in discrete magnetospheric flaring? These emission mechanisms produce different spectral or temporal signatures, which can be distinguished using the EPIC imagers in concert with ground-based photometry and spectroscopy. If due to accretion, we expect the X-ray flux to correlate with the instantaneous mass accretion rate. Our AO4 observations of RU Lupi show a clear correlation between the optical and X-ray brightness, but the interpretation is not yet clear. The result of this program will be a better understanding of the coronae of the youngest low mass stars.

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