Long-term timing of the relativistic binary PSR J1906+0746

ABSTRACT We conducted a timing analysis of over 18 yr of data on the young ($\tau _{\rm c} = 112$ kyr, $P = 114$ ms) relativistic binary PSR J1906+0746, using six radio telescopes: Arecibo, FAST, Green Bank, Lovell, MeerKAT, and Nançay. This pulsar is known to orbit a compact high-mass companion with a period of 3.98 h in a mildly eccentric orbit ($e = 0.085$). By combining all data and maintaining a coherent timing solution over the full span, we obtained a more precise measurement of the advance of periastron, $\dot{\omega } = 7.5841(2)$ $\deg$ yr$^{-1}$, the Einstein delay, $\gamma = 4.59(2) \times 10^{-4}$ s, and the secular change in orbital period, $\dot{P}_{\rm b} = -5.65(2) \times 10^{-13}$ s s$^{-1}$. Assuming the validity of general relativity, we obtain a total mass of 2.6133(1) ${\rm M}_{\odot }$ and component masses of 1.316(5) ${\rm M}_{\odot }$ for the pulsar and 1.297(5) ${\rm M}_{\odot }$ for the companion, consistent with a double neutron star system. However, when fitting for the secular change in the projected semimajor axis we obtain $\dot{x} = -1.8(6) \times 10^{-13}$ s s$^{-1}$. The component masses are shifted by $\sim 3.5\sigma$, which is expected from the correlation of $\dot{x}$ and $\gamma$. The $\dot{x}$ has a similar magnitude to that observed in PSR J1141–6545, which is due to spin–orbit coupling; if confirmed, it would indicate that, as in the latter system, the companion of the PSR J1906+0746 system is a massive fast-rotating white dwarf formed before the pulsar. Additionally, we report and characterize a large glitch near MJD 56664, with a fractional frequency increase comparable to those observed in the Vela pulsar.