2004ApJ...613L..53C

We report on a 50 ks XMM-Newton observation of the double pulsar system J0737-3039 performed in 2004 April. We present results of the spectral analysis of these data combined with the much shorter Chandra pointing performed in 2004 January. Blackbody emission with an effective temperature of 0.20^+0.02_–0.02keV (90% confidence level) and emission radius 75⁺³⁰_–9 m for a distance of 0.5 kpc (implying a 0.5-10 keV luminosity ∼6x10²⁹ ergs/s) is a viable interpretation, calling for a stream of particles accelerated in the magnetosphere of PSR J0737-3039A and depositing their kinetic energy in the magnetic polar cap of PSR J0737-3039A or of the companion PSR J0737-3039B. A single power-law emission model implies a very steep photon index Γ=4.2^+2.1_–1.2 and a suspiciously high hydrogen column density, whereas a photon index Γ=2 does not provide an adequate description of the XMM-Newton and Chandra data. A two-component model (a blackbody plus a power law with Γ=2) is statistically acceptable, but the additional power-law component is not required by the data.