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We observed the double neutron star binary (DNSB) containing PSR J1537+1155(also known as B1534+12) with the Chandra X-ray Observatory. This is one of thetwo DNSBs detected in X-rays and the only one where a hint of variability withorbital phase was found (in the previous Chandra observation). Our follow-upobservation supports the earlier result: the distribution of photon arrivaltimes with orbital phase again shows a deficit around apastron. Thesignificance of the deficit in the combined dataset exceeds 99%. Such anorbital light-curve suggests that the X-ray emission is seen only when neutronstar B passes through the equatorial pulsar wind of neutron star A. We describestatistical tests we used to determine the significance of the deficit, andconclusions that can be drawn from its existence, such as interaction of thepulsar wind with the neutron star companion. We also provide better constrainedspectral model parameters obtained from the joint spectral fits to the datafrom both observations. A power-law successfully fits the data, with best-fitphoton index Gamma=3.1pm0.4 and unabsorbed flux f=(3.2pm0.8)x10^-15 erg s-1cm-2(0.3-8 keV range).

Orbital variation of the X-ray emission from the double neutron star binary J1537+1155