Radio eclipse of the slowest spinning Galactic-field spider pulsar PSR J1932+2121 and its X-ray emission prospect
Abstract
PSR J1932+2121 is a newly discovered spider pulsar with a pronounced radio eclipse identified by the Five-hundred-meter Aperture Spherical radio Telescope (FAST); it provides an ideal laboratory for studying the eclipse mechanism and high-energy emission from its intrabinary shock (IBS). By modeling the orbital-phase-dependent dispersion measure variations and flux profiles during the eclipse region with the wind interaction and IBS geometry, we constrain the system to a nearly edge-on inclination (io 88.55) and a weak stellar wind from a low-mass main-sequence companion. Our analysis of the eclipse mechanism suggests that synchrotron absorption by nonthermal electrons can reproduce the observed flux variations with reasonable parameters for the eclipsing medium. We further predict the synchrotron emission from the IBS in PSR J1932+2121, showing that its X-ray flux, particularly near the inferior conjunction of the companion star, could be detectable with XMM/EPIC, EP/FXT, or eXTP/SFA and should exhibit double-peaked orbital modulation by Doppler boosting. These results provide a theoretical framework for understanding this system and for guiding future multiwavelength probes of spider pulsars.
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