Apparently ultra-long period radio sources from self-lensed pulsar-black hole binaries

Pulsar-black hole (BH) close binary systems, which have not been found yet, are unique laboratories for testing theories of gravity and understanding the formation channels of gravitational-wave sources. We study the self-gravitational lensing effect in a pulsar-BH system on the pulsar's emission. Because this effect occurs once per orbital period for almost edge-on binaries, we find that it could generate apparently ultra-long period (minutes to hours) radio signals when the intrinsic pulsar signal is too weak to detect. Each of such lensed signals, or 'pulse', is composed of a number of amplified intrinsic pulsar pulses. We estimate that a radio telescope with a sensitivity of \(10\,\rm mJy\) could detect \(\sim\) a few systems that emit such signals in our galaxy. The model is applied to three recently found puzzling long-period radio sources: GLEAM-X J1627, PSR J0901-4046, and GPM J1839-10. To explain their observed signal durations and periods, the masses of their lensing components would be \(\sim10^4\,\rm M_{\odot}\), \(\sim4\,\rm M_{\odot}\) and \(10^{3-6}\,\rm M_{\odot}\), respectively, with their binary coalescence times ranging from a few tens to thousands of years. However, the implied merger rates (as high as \(\sim 10^{3-4}\,\rm Myr^{-1}\) per galaxy) and the large period decay rates (\(>10^{-8}\,\rm s\,s^{-1}\)) tend to disfavour this self-lensing scenario for these three sources. Finally, for a binary containing a millisecond pulsar and a stellar-mass BH, the Shapiro delay effect would cause a \(\geq10\%\) variation of the profile width for the sub-pulses in such lensed signals.