A highly resistive layer within the crust of X-ray pulsars limits their spin periods

TL;DR

This paper proposes that a highly resistive, amorphous inner crust in neutron stars naturally limits X-ray pulsars' spin periods to about 10-20 seconds, explaining the observed absence of longer-period pulsars.

Contribution

It introduces the concept that an amorphous, heterogeneous inner crust causes a resistive layer that caps pulsar spin periods, providing a potential observational signature of crust composition.

Findings

Resistive layer limits pulsar spin periods to 10-20 seconds.

Amorphous crust phase linked to nuclear pasta may cause high resistivity.

Maximum period observations can constrain neutron star crust properties.

Abstract

The lack of X-ray pulsars with spin periods > 12 s raises the question of where the population of evolved high magnetic field neutron stars has gone. Unlike canonical radio pulsars, X-ray pulsars are not subject to physical limits to the emission mechanism nor observational biases against the detection of sources with longer periods. Here we show that a highly resistive layer in the innermost part of the crust of neutron stars naturally limits the spin period to a maximum value of about 10-20 s. This highly resistive layer is expected if the inner crust is amorphous and heterogeneous in nuclear charge, possibly due to the existence of a nuclear pasta phase. Our findings suggest that the maximum period of isolated X-ray pulsars can be the first observational evidence of an amorphous inner crust, which properties can be further constrained by future X-ray timing missions combined with more detailed models.