On the origin of the quasi-periodic micro-pulses observed in the radio-frequency emission of some neutron stars

TL;DR

This paper explores the origin of quasi-periodic micro-pulses in neutron star radio emissions, linking micro-pulse widths to neutron star surface physics and plasma instabilities.

Contribution

It proposes a physical model connecting micro-pulse widths to a specific surface area supporting plasma instabilities in neutron stars.

Findings

Micro-pulse widths scale with neutron star rotation period

A physical length on the neutron star surface influences emission properties

Ion-proton plasma instabilities drive the observed radio micro-pulses

Abstract

The linear relationship between pulsar micro-pulse widths and rotation period is consistent with the existence of a physical length L on the neutron-star surface and seen on the observer arc of transit across the polar cap. Within the ion-proton model it is the width of the minimum area of surface that can support the critical growth rate of the unstable two-beam Langmuir mode that is the source of the radio emission.