XMM-Newton Proposal 03039002

Details XMM-Newton Proposal 03039002 XMM-Newton Proposal 03039002

Oct 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004xmm..prop..137w&link_type=abstract

XMM-Newton Proposal ID #03039002

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Stars, White Dwarfs, Solar System, Ru Lup, Xmm-Newton Proposal 03039002

Scientific paper

What is the nature of the weak X-ray emission observed in the ``continuum'' T Tauri stars, low mass PMS stars with large mass accretion rates? Do they 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 three emission mechanisms produce different spectral or temporal signatures, which can be distinguished using the EPIC imagers in concert with ground-based photometry. If due to accretion, we expect the X-ray flux to correlate with the instantaneous mass accetion rate. We choose three targets that we have been following. The result of this program will be a better understanding of the coronae and magnetic fields in the youngest low mass stars.

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