PSR J1024 - 0719 is a millisecond pulsar that was long thought to be isolated .
However , puzzling results concerning its velocity , distance , and low rotational period derivative have led to reexamination of its properties .
We present updated radio timing observations along with new and archival optical data that show PSR J1024 - 0719 is most likely in a long period ( 2–20 kyr ) binary system with a low-mass ( \approx 0.4 M _ { \odot } ) low-metallicity ( Z \approx - 0.9 dex ) main sequence star .
Such a system can explain most of the anomalous properties of this pulsar .
We suggest that this system formed through a dynamical exchange in a globular cluster that ejected it into a halo orbit , consistent with the low observed metallicity for the stellar companion .
Further astrometric and radio timing observations such as measurement of the third period derivative could strongly constrain the range of orbital parameters .