We report the discovery with XMM-Newton of 3 s X-ray pulsations from 3XMM J004232.1+411314, a dipping source that dominates the hard X-ray emission of M31. This finding unambiguously assesses the neutron star (NS) nature of the compact object. We also measured an orbital period of 4.15 hr and a projected semi-axis at aX sin i = 0.6 lt-s, which implies a low-mass companion of about 0.2-0.3 M ⊙ assuming an NS of 1.5 M ⊙ and an orbital inclination i = 60°-80°. The barycentric orbit-corrected pulse period decreased by ˜28 ms in about 16 year, corresponding to an average spin-up rate of dot{P}˜ -6× {10}-11 s s-1 pulse period variations, probably caused by X-ray luminosity changes, were observed on shorter timescales. We identify two possible extreme scenarios for the source: a mildly magnetic NS with B p ≃ few × 1010 G if the pulsar is far from its equilibrium period P eq and the disk is truncated at the value of the Alfvén radius corresponding to the observed luminosity, and a relatively young, highly magnetic NS with B eq ≃ 2 × 1013 G if spinning close to P eq and the disk is truncated close to the co-rotation surface.

Discovery of a 3 s Spinning Neutron Star in a 4.15 hr Orbit in the Brightest Hard X-Ray Source in M31

Esposito P.;Tiengo A.;De Luca A.;Marelli M.
2018

Abstract

We report the discovery with XMM-Newton of 3 s X-ray pulsations from 3XMM J004232.1+411314, a dipping source that dominates the hard X-ray emission of M31. This finding unambiguously assesses the neutron star (NS) nature of the compact object. We also measured an orbital period of 4.15 hr and a projected semi-axis at aX sin i = 0.6 lt-s, which implies a low-mass companion of about 0.2-0.3 M ⊙ assuming an NS of 1.5 M ⊙ and an orbital inclination i = 60°-80°. The barycentric orbit-corrected pulse period decreased by ˜28 ms in about 16 year, corresponding to an average spin-up rate of dot{P}˜ -6× {10}-11 s s-1 pulse period variations, probably caused by X-ray luminosity changes, were observed on shorter timescales. We identify two possible extreme scenarios for the source: a mildly magnetic NS with B p ≃ few × 1010 G if the pulsar is far from its equilibrium period P eq and the disk is truncated at the value of the Alfvén radius corresponding to the observed luminosity, and a relatively young, highly magnetic NS with B eq ≃ 2 × 1013 G if spinning close to P eq and the disk is truncated close to the co-rotation surface.
galaxies: individual: M31, stars: neutron, X-rays: binaries, X-rays: individual: 3XMM J004232.1+411314, CXOM31 J004232.0+411314, Swift J0042.6+4112
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/20.500.12076/4904
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