Magneto-rotational and thermal evolution of young neutron stars

TL;DR

This paper reviews neutron star populations, focusing on the period dichotomy among nearby cooling neutron stars, and proposes a bimodal magnetic field distribution linked to magnetar formation as a potential explanation.

Contribution

It introduces the idea that a bimodal initial magnetic field distribution can explain the observed period dichotomy in young neutron stars.

Findings

Two distinct groups of neutron stars with different spin periods are observed.

A bimodal magnetic field distribution may account for the period differences.

The proposed model links magnetar formation mechanisms to neutron star evolution.

Abstract

After a brief review of population synthesis of close-by cooling neutron stars, I focus on the interpretation of dichotomy of spin periods of near-by coolers. The existence of two well separated groups -- short period ($\sim$0.1-0.3 s) radio pulsars and long period ($\sim$3-10 s) radio quiet sources, aka the Magnificent seven, -- can not be easily explained in unified models developed recently (Popov et al. 2010, Gull{\'o}n et al. 2014). I speculate that the most natural solution of the problem can be in bimodal initial magnetic field distribution related to the existence of an additional mechanism of field generation in magnetars.