2024A&A...691A..22G

Context. PSR J1618-3921 is one of five known millisecond pulsars (MSPs) in eccentric orbits (eMPSs) located in the Galactic plane, whose formation is poorly understood. Earlier studies of these objects revealed significant discrepancies between observations and predictions from standard binary evolution scenarios of pulsar-helium white dwarf (HeWD) binaries, especially in the case of PSR J0955-6150, for which mass measurements ruled out most eMSP formation models.
Aims. We aim to measure the masses of the pulsar and its companion, and constrain the orbital configuration of PSR J1618-3921. This facilitates understanding similarities among eMSPs and could offer hints as to their formation mechanism.
Methods. We conducted observations with the L-band receiver of the MeerKAT radio telescope and the UWL receiver of the Parkes Murriyang radio telescope between 2019 and 2021. These data were added to archival Parkes and Nançay observations. We performed a full analysis on this joint data set with a timing baseline of 23 years. We also used the data from recent observations to give a brief account of the emission properties of J1618-3921, including a rotating vector model (RVM) fit of the linear polarisation position angle of the pulsar.
Results. From the timing analysis, we measure a small but significant proper motion of the pulsar. The long timing baseline allowed for a highly significant measurement of the rate of advance of periastron of $ \dot{\omega} = (0.00145 \pm 0.00010)\circ\mathrm{yr}^{-1} $. Despite the tenfold improvement in timing precision from MeerKAT observations, we can only report a low-significance detection of the orthometric Shapiro delay parameters, $ h_3 = 2.70^{+2.07}_{-1.47}\, {\upmu}\mathrm{s} $ and $ \varsigma = 0.68^{+0.13}_{-0.09} $. Under the assumption of the validity of general relativity (GR), the self-consistent combination of these three parameters leads to mass estimates of the total and individual masses in the binary of $ M_{\mathrm{tot}}= 1.42^{+0.20}_{-0.19}\,\mathrm{M}_{\odot} $, $ M_{\mathrm{c}} = 0.20^{+0.11}_{-0.03}\,\mathrm{M}_{\odot} $, and $ M_{\mathrm{p}} = 1.20^{+0.19}_{-0.20}\,\mathrm{M}_{\odot} $. We detect an unexpected change in the orbital period of $ \dot{P}_{\mathrm{b}} =-2.26^{+0.35}_{-0.33}\,\times\, 10^{-12} $, that is an order of magnitude larger and carries an opposite sign to what is expected from the Galactic acceleration and the Shklovskii effect, which are a priori the only non-negligible contributions expected for Ṗ_b. We also detect a significant second derivative of the spin frequency, $ \ddot{f} $. The RVM fit reveals a viewing angle of ζ = (111 ± 1)°. Furthermore, we report an unexpected, abrupt change in the mean pulse profile in June 2021 of unknown origin.
Conclusions. We propose that the anomalous Ṗ_b and $ \ddot{f} $ we measure for J1618-3921 indicate an additional varying acceleration due to a nearby mass. The J1618-3921 binary system is likely part of a hierarchical triple, but with the third component much farther away than the outer component of the MSP in a triple star system, PSR J0337+1715. This finding suggests that at least some eMSPs might have formed in triple star systems. Although the uncertainties are large, the binary companion mass is consistent with the P_b - M_WD relation, which has been verified for circular HeWD binaries and also for the two HeWDs in the PSR J0337+1715 system. Future regular observations with the MeerKAT telescope will, due to the further extension of the timing baseline, improve the measurement of Ṗ_b and $ \ddot{f} $. This will help us further understand the nature of this system, and perhaps improve our understanding of eMSPs in general.