http://arxiv.org/abs/2002.01920
The 16 days periodicity observed in FRB 180916.J0158+65 by the CHIME telescope is consistent with a tight, stellar mass binary system of semi-major axis $\sim 10^{12}$ cm. The primary is an early B-type star with mass loss rate $\dot{M} \sim 10^{-8}- 10^{-10} M_\odot$ yr$^{-1}$. The observed periodicity is not intrinsic to the FRBs’ source, but is due to the orbital phase-dependent modulation of the absorption conditions in the B-star’s wind. Relatively narrow activity window implies that the companion’s wind dynamically dominates the pulsar wind, $\eta = L_{sd}/(\dot{M} v_w c) \leq 1$, where $L_{sd} $ is pulsar spin-down, $\dot{M}$ is companion’s wind mass loss rate and $v_w$ is its velocity. More massive O stars produce denser wind that are optically thick to radii much large than the the orbital separation. Condition $\eta \leq 1$ requires mildly powerful pulsar with $L_{sd} \sim 10^{34}-10^{36}$ erg $s^{1}$. The observations are consistent with magnetically-powered radio emission originating in the magnetospheres of strongly magnetized neutron stars, the classical magnetars.
M. Lyutikov, M. Barkov and D. Giannios
Thu, 6 Feb 20
57/57
Comments: N/A