The Timing and Polarization of PSR J0002+6216

Abstract The combined timing analysis of data from the Five-hundred-meter Aperture Spherical radio Telescope (FAST) and the Fermi Large Area Telescope confirmed that PSR J0002+6216 is not a hyper-velocity (exceeding 1000 km s −1 ) pulsar. From this analysis, we determined the total proper motion of PSR J0002+6216 to be μ tot = 39.05 ± 15.79 mas yr −1 , which is consistent with Very Long Baseline Interferometry (VLBI) measurements to within 0.24 σ . Moreover, two glitches were detected for the first time, which occurred on MJD 58850(17) and MJD 60421(6), respectively. The second glitch exhibited an exponential recovery process, with Q = 0.0090(3) and τ d = 45(3) days. Additionally, with FAST high-sensitivity observations, we measured the interstellar rotation measure (RM) and the 3D orientation of the spin axis for the first time, and updated the dispersion measure (DM) of PSR J0002+6216. Currently, no variations in RM or DM have been detected. By combining the measured RM with the observed position angle of the spin axis, we determined that the intrinsic position angle of the pulsar’s spin axis is <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msub> <mml:mi>ψ</mml:mi> <mml:mn>0</mml:mn> </mml:msub> <mml:mo stretchy="false">(</mml:mo> <mml:mi>intrinsic</mml:mi> <mml:mo stretchy="false">)</mml:mo> <mml:mo>=</mml:mo> <mml:mn>89</mml:mn> <mml:mover accent="true"> <mml:mi>.</mml:mi> <mml:mi>°</mml:mi> </mml:mover> <mml:mn>9</mml:mn> <mml:mo>±</mml:mo> <mml:mn>4</mml:mn> <mml:mover accent="true"> <mml:mi>.</mml:mi> <mml:mi>°</mml:mi> </mml:mover> <mml:mn>6</mml:mn> </mml:math> . When we compared this with the proper motion position angle obtained from VLBI, we found a misalignment of approximately 23 ∘ between the spin and velocity angles of PSR J0002+6216. At present, pulsars with 2D spin–velocity angle measurements are unable to fully test the Janka et al. model. However, with more high-precision observational data in the future, we will be able to further test models related to pulsar birth.