X-ray Emission from the Double Neutron Star Binary B1534+12: Powered by the Pulsar Wind?

We report the detection of the double neutron star binary (DNSB) B1534+12 (= J1537+1155) with the Chandra X-ray Observatory. This DNSB (Porb = 10.1 hr) consists of the millisecond (recycled) pulsar J1537+1155A (PA = 37.9 ms) and a neutron star not detected in the radio. After the remarkable double pulsar binary J0737−3039, it is the only other DNSB detected in X-rays. We measured the flux of (2.2 ± 0.6)× 10 ergs s cm in the 0.3–6 keV band. The small number of collected counts allows only crude estimates of spectral parameters. The power-law fit yields the photon index Γ = 3.2 ± 0.5 and the unabsorbed 0.2–10 keV luminosity LX ≈ 6 × 10 29 ergs s ≈ 3 × 10ĖA, where ĖA is the spin-down power of J1537+1155A. Alternatively, the spectrum can be fitted by a blackbody model with T ≈ 2.2 MK and the projected emitting area of ∼ 5×10 m. The distribution of photon arrival times over binary orbital phase shows a deficit of X-ray emission around apastron, which suggests that the emission is caused by interaction of the relativistic wind from J1537+1155A with its neutron star companion. We also reanalyzed the Chandra and XMM-Newton observations of J0737−3039 and found that its X-ray spectrum is similar to the spectrum of B1534+12, and its X-ray luminosity is about the same fraction of ĖA, which suggests similar X-ray emission mechanisms. However, the X-ray emission from J0737−3039 does not show orbital phase dependence. This difference can be explained by the smaller eccentricity of J0737−3039 or a smaller misalignment between the equatorial plane of the millisecond pulsar and the orbital plane of the binary. Subject headings: pulsars: individual (PSR B1534+12 = PSR J1537+1155, PSR J0737−3039A, PSR J0737−3039B) — stars: neutron — X-rays: stars