Abstract
Typical radio pulsars are magnetized neutron stars that are born rapidly rotating and slow down as they age on time scales of 10 to 100 million years. In contrast, millisecond radio pulsars spin very rapidly even though many are billions of years old1. The most compelling explanation is that they have been ‘spun up’ by the transfer of angular momentum during the accretion of material from a companion star in so-called low-mass X-ray binary systems, LMXBs. (LMXBs consist of a neutron star or black hole accreting matter from a companion with mass less than one solar mass2.) The recent detection of coherent X-ray pulsations with a millisecond period from a suspected low-mass X-ray binary system appears to confirm this link3. Here we report observations showing that the orbital period of this binary system is two hours, which establishes it as an LMXB. We also find an apparent modulation of the X-ray flux at the orbital period (at the two per cent level), with a broad minimum when the pulsar is behind the low-mass companion star. This system seems closely related to the ‘black-widow’ millisecond radio pulsars, which are evaporating their companions through irradiation4,5,6,7,8. It may appear as an eclipsing radio pulsar during periods of X-ray quiescence.
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Acknowledgements
We thank L. Bildsten, V. Kaspi, A. Levine, R. Nelson, R. Remillard, F. Rasio, S.Thorsett, M. van der Klis and B. Vaughan for discussions, and M. Muno for assistance with the data analysis. We also thank F. Marshall, J. Swank and the RXTE team at NASA/Goddard Space Flight Center for arranging these target-of-opportunity observations and the necessary follow-up. This work was supported by NASA.
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Chakrabarty, D., Morgan, E. The two-hour orbit of a binary millisecond X-ray pulsar. Nature 394, 346–348 (1998). https://doi.org/10.1038/28561
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DOI: https://doi.org/10.1038/28561
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