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We present the X-ray grating spectra of the recurrent nova RS Ophiuchi duringits 2006 outburst, obtained with the XMM-Newton and Chandra observatories. Twoweeks after optical maximum, the X-ray spectrum was hard and dominated byemission lines of H-like and He-like ions. The X-ray luminosity was 2.4 x 10^36erg s^-1 in the 0.33-10 keV range. The spectra indicate a collisionallydominated plasma with a broad range of temperatures. All the lines areblue-shifted, with the velocity shift increasing with lower ionization stateand longer wavelength. Two weeks later, the spectrum was still dominated byemission lines, although the line ratios present indicate cooling. During thisobservation, a soft X-ray flare occurred in which a new system of highervelocity emission lines appeared in the soft end of the spectrum. The dominantcomponent during the third month was the supersoft continuum with the broadabsorption features of a hot white dwarf atmosphere. A preliminary model fitindicates a white dwarf temperature slightly exceeding 800,000 K. The X-rayluminosity reached at least 9 x 10^37 erg s^-1 in the 0.2-1 keV range, whilethe intrinsic nebular absorption decreased by a factor of five since the firstobservation. The spectral fits indicate a massive white dwarf, with a mass ofat least 1.2 M_\odot. Therefore, RS Oph may be an important type Ia supernovaprogenitor. We show that the data are consistent with mass loss ending beforeday 54 after the outburst, and nuclear burning ending around day 69. A rapiddecay in X-ray luminosity followed after week 10. The X-ray luminosity 5, 7 and8 months after optical maximum dropped by more than two orders of magnitude.The spectra do not appear to consistent with emission from an accretion disk.

X-ray Spectroscopy of the 2006 Outburst of RS Oph