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Chasing coronal x-ray emission to the end of the pleiades main sequence.... and beyond?

By K. R. Briggs and J. P. Pye

Abstract

We have used a 40-ks XMM-Newton observation to examine the X-ray emission of 33 proposed M-type members in. the core of the Pleiades. We reach a limiting X-ray luminosity of LX ≈ × 1027 erg s−1 in the field centre and detect 17 of 19 members with MIc < 10.5 (where MIc is absolute magnitude in the Cousins I band, which is centered on 790 nm), and 2 of 14 fainter members. A further possible detection of the brown dwarf candidate Roque 9, with log LX ≈ 27.8 and X-ray-to-bolometric luminosity ratio of Full-size image (<1 K), may be due to a chance alignment with a background source. Although the X-ray luminosity decreases sharply with increasing MIc (later-types, lower-masses), all but 3 members show LX consistent with near-saturated emission and we do not see convincing evidence for a decrease in activity level indicative of a decrease in dynamo efficiency at the spectral type at which stellar structure is expected to become fully-convective

Year: 2003
DOI identifier: 10.1016/S0273-1177(03)00310-7
OAI identifier: oai:lra.le.ac.uk:2381/742
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