Is the high mass binary pulsar PSR J 1614-2230 a latent magnetar?

TL;DR

This paper explores why the high mass binary pulsar PSR J1614-2230 does not exhibit magnetar characteristics, proposing that slow accretion limits magnetic field emergence despite its high mass.

Contribution

It introduces a model explaining the latent magnetar state of PSR J1614-2230 based on energy gain rates and temperature constraints during accretion.

Findings

Energy gain from phase transition is insufficient for magnetic field emergence.

High mass alone does not guarantee magnetar characteristics.

Slow accretion prevents magnetic field transport to the surface.

Abstract

We consider the newly found high mass and low magnetic field binary pulsar PSR J1614-2230 in a model in which magnetars owe their strong magnetic fields to a high baryon density, magnetized core. In our magnetar model all neutron stars above a certain threhold mass are magnetars. This confronts us with the very basic paradox as to why this high mass star, PSR J1614-2230, remains a pulsar and shows no magnetar characteristics. This is a star that has acquired its large mass by accretion from its binary companion over 5 gigayears. In this work we show that the maximum rate of energy gain from the strong interaction phase transition from this slow accretion does not allow for high enough interior temperature for ambipolar transport of the magnetic field to the surface of the star and thus the PSR J 1614-2230 remains latent and does not become an emergent magnetar.