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We present the high-resolution RGS X-ray spectrum of the stellar binary Capella observed by the XMM- Newton satellite. A multi-thermal approach has rst been applied to t the data and derive elemental abundances. Using the latter, the emission measure distribution has been reconstructed using a Chebychev polynomial t. Its shape is found to display a sharp peak around 7 MK, consistent with previous EUVE and ASCA results. A smaller but signicant amount of emission measure is required around 1.8 MK in order to explain the O vii He-like triplet and the C vi Ly line. We have applied the temperature diagnostics of dielectronic recombination satellite lines to the He-like O vii triplet to constrain the cool plasma temperature, and have obtained a lower limit consistent with the global reconstruction of the emission measure distribution. We have used line ratios from the forbidden, intercombination, and resonance lines of the O vii triplet to derive an average density for the cool coronal plasma (ne < 11 0 10 cm 3 ). Implications for the coronal structure of Capella are discussed.

The XMM-Newton view of stellar coronae: High-resolution X-ray spectroscopy of Capella