Kavli Affiliate: Lijing Shao
| First 5 Authors: Lingqi Meng, Weiwei Zhu, Michael Kramer, Xueli Miao, Gregory Desvignes
| Summary:
We observe systematic profile changes in the visible pulsar of the compact
double neutron star system PSR~J1946+2052 using observations with the
Five-hundred-meter Aperture Spherical radio Telescope (FAST). The interpulse of
PSR~J1946+2052 changed from single-peak to double-peak shape from 2018 to 2021.
We attribute this evolution as the result of the relativistic spin precession
of the pulsar. With the high sensitivity of FAST, we also measure significant
polarization for the first time, allowing us to model this with the
precessional rotating vector model. Assuming, to the first order, a circular
hollow-cone-like emission beam pattern and taking the validity of general
relativity, we derive the binary’s orbital inclination angle
(${63^circ}^{+5^circ}_{-3^circ}$) and pulsar’s spin geometry. Pulsar’s spin
vector and the orbital angular momentum vector are found to be only slightly
misaligned (${0.21^circ}^{+0.28^circ}_{-0.10^circ}$).The quoted
uncertainties do not reflect the systematic uncertainties introduced by our
model assumptions. By simulating future observations of profile and
polarization evolution, we estimate that we could constrain the precession rate
within a $43%$ uncertainty in 9 years. Hence, we suggest that the system’s
profile evolution could be combined with precise pulsar timing to test general
relativity in the future.
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