Pulsar glitch and nuclear EoS: Applicability of superfluid model
A. Li, R. Wang
TL;DR
This paper evaluates contemporary neutron star equations of state against pulsar glitch constraints, suggesting that certain models align with observed data and may resolve the glitch crisis.
Contribution
It assesses the applicability of superfluid models to neutron star glitches using modern EOSs and recent observational constraints.
Findings
Neutron star radii are around 12.5 km for selected pulsars.
Stars with mass less than 1.55 solar masses meet glitch constraints.
The glitch crisis might be resolved with current superfluid models.
Abstract
In this contribution, we have made use of the contemporary equation of states (EOSs) for the complete neutron star structure, and confronted them with one particular glitch constrain for the crustal moment of inertia (MOI). We find that with these EOSs, the radii of three millisecond pulsars selected by NICER: PSR J0437-4715, PSR J1614-2230, PSR J0751+1807, are all around 12.5 km. Also, a star with would fulfill the MOI calculation for glitch constrain with the latest neutron superfluidity density, and the glitch crisis might not be present.
Peer Reviews
No public reviews on file for this paper yet. If you reviewed it on a platform where reviews are public (OpenReview, ICLR, NeurIPS, ICML), you can paste yours below so the community can read it here.
Videos
No videos yet. Explain this paper in a talk, walkthrough, or lecture? Add one.