Long-Term Radio Timing Observations of the Transition Millisecond Pulsar PSR~J1023+0038

TL;DR

This study presents four years of radio timing observations of the pulsar PSR J1023+0038, revealing complex eclipse behavior, orbital variations, and gamma-ray modulation, challenging existing models of the companion's magnetic activity.

Contribution

The paper provides the first long-term timing solution for PSR J1023+0038 and interprets eclipse phenomena and orbital variations in terms of magnetic activity and gravitational quadrupole coupling.

Findings

Detected variable eclipses and excess dispersion measure near eclipses.

Found no orbital modulation of gamma-ray emission, but detected pulsar-period modulation.

Suggested magnetic activity in the companion influences orbital period variations.

Abstract

The radio millisecond pulsar PSR J1023+0038 exhibits complex timing and eclipse behavior. Here we analyze four years' worth of radio monitoring observations of this object. We obtain a long-term timing solution, albeit with large residual timing errors as a result of apparent orbital period variations. We also observe variable eclipses when the companion passes near our line of sight, excess dispersion measure near the eclipses and at random orbital phases, and short-term disappearances of signal at random orbital phases. We interpret the eclipses as possibly due to material in the companion's magnetosphere supported by magnetic pressure, and the orbital period variations as possibly due to a gravitational quadrupole coupling mechanism. Both of these mechanisms would be the result of magnetic activity in the companion, in conflict with evolutionary models that predict it should be fully convective and hence non-magnetic. We also use our timing data to test for orbital and rotational modulation of the system's $\gamma$-ray emission, finding no evidence for orbital modulation and $3.7\sigma$ evidence for modulation at the pulsar period. The energetics of the system make it plausible that the $\gamma$-ray emission we observe is entirely from the millisecond pulsar itself, but it seems unlikely for these $\gamma$-rays to provide the irradiation of the companion, which we attribute instead to X-ray heating from a shock powered by a particle wind.