How Massive Are the Superfluid Cores in the Crab and Vela Pulsars and Why Their Glitch-Events Are Accompanied with under and Overshootings?

A A Hujeirat,R Samtaney

doi:10.4236/jmp.2020.113025

Abstract

The Crab and Vela are well-studied glitching pulsars and the data obtained sofar should enable us to test the reliability of models of their internal structures. Very recently it was proposed that glitching pulsars are embedded in bimetric spacetime: their incompressible superfluid cores (SuSu-cores) are embedded in flat spacetime, whereas the ambient compressible and dissipative media are enclosed in Schwarzschild spacetime. In this letter we apply this model to the Crab and Vela pulsars and show that a newly born pulsar initially of $1.25\text{M}_{\odot}$ and an embryonic SuSu-core of $0.029\text{M}_{\odot}$ could evolve into a \ARZL{Crab-like}\ARZR pulsar after 1000 years and into a \ARZL{Vela-like}\ARZR pulsar 10000 years later to finally fade away as an invisible dark energy object after roughly 10 Myr. Based thereon we infer that the Crab and the Vela pulsars should have SuSu-cores of $0.15\text{M}_{\odot}$ and $0.55\text{M}_{\odot}$, respectively. Futhermore, the under- and overshootings phenomena observed to accompany the glitch events of the Vela pulsar are rather a common phenomenon of glitching pulsars that can be well-explained within the framework of bimetric spacetime.

Highlights

E into a Crab-like pulsar after 1000 years and into a Vela-like pulsar 10,000 years later to fade away as an invisible dark energy object after roughly
The Crab and Vela are well-studied glitching pulsars and the data obtained so far should enable us to test the reliability of models of their internal structures
Very recently it was proposed that glitching pulsars are embedded in bimetric spacetime: their incompressible superfluid cores (SuSu-cores) are embedded in flat spacetime, whereas the ambient compressible and dissipative media are enclosed in Schwarzschild spacetime

Summary

Introduction

E into a Crab-like pulsar after 1000 years and into a Vela-like pulsar 10,000 years later to fade away as an invisible dark energy object after roughly. This approach is more consistent than the former, as the elements of ∆Ωncr are determined here through the rate of loss of rotational energy of the entire star and that these should overlap the current values observed in the Crab and Vela pulsars.

Results

Conclusion