Evolutionary Origin of Ultralong-period Radio Transients

Abstract

Recently, two ultralong-period radio transients, GLEAM-X J162759.5-523504.3 (J1627) and GPM J1839-10 (J1839), were discovered with spin periods longer than 1000 s. The origin of these two ultralong-period radio transients is intriguing in understanding the spin evolution of neutron stars (NSs). In this work, we examine whether the interaction between strong magnetized NSs and fallback disks can spin NSs down to the observed ultralong period. Our simulations found that the magnetar + fallback disk model can account for the observed period, period derivative, and X-ray luminosity of J1627 in the quasi-spin-equilibrium stage. To evolve to the current state of J1627, the initial mass-accretion rate of the fallback disk and the magnetic field of the NS are in the range of (1.1–30) × 1024 g s−1 and (2–5) × 1014 G, respectively. In the active lifetime of the fallback disk, it is impossible for J1839 to achieve the observed upper limit of the period derivative. Therefore, we propose that J1839 may be in the second ejector phase after the fallback disk becomes inactive. Those NSs with a magnetic field of (2–6) × 1014 G and a fallback disk with an initial mass-accretion rate of ∼1024–1026 g s−1 are possible progenitors of J1839.

On the Interacting/Active Lifetime of Supernova Fallback Disks around Isolated Neutron Stars

“…Considering that the corotation radius R c and the light cylinder radius R lc are relative to the spin period of an NS, the spin evolution is also simulated. 9 Our simplified propeller form does not differ significantly from others, e.g., Fan et al (2024). 10 The disk undergoes neutralization when its temperature is lower than the critical value of T C ∼ 6500 K (Menou et al 2001).…”