What question did this study set out to answer?

This research aims to explore the implications of wave-function collapse models on the heating of neutron stars.

August 21, 2019Open Access

Neutron Star Heating Constraints on Wave-Function Collapse Models

Key Points

This research aims to explore the implications of wave-function collapse models on the heating of neutron stars.
Calculated collapse-induced heating rates for astrophysical objects, particularly neutron stars.
Derived equilibrium temperatures and assessed bounds using observational data from neutron stars.
Proposed additional speculative bounds based on current and future astronomical survey capabilities.
Heating rates increase with stronger collapse model parameters, indicating significant energy shifts in neutron stars.
Competitive bounds on model parameters derived from the observational data of neutron stars suggest limits on collapse models.
Speculative bounds proposed for future observations could refine these constraints further.

Abstract

Spontaneous wave-function collapse models, like continuous spontaneous localization, are designed to suppress macroscopic superpositions while preserving microscopic quantum phenomena. An observable consequence of collapse models is spontaneous heating of massive objects. We calculate the collapse-induced heating rate of astrophysical objects, and the corresponding equilibrium temperature. We apply these results to neutron stars, the densest phase of baryonic matter in the Universe. Stronger collapse model parameters imply greater heating, allowing us to derive competitive bounds on model parameters using neutron star observational data, and to propose speculative bounds based on the capabilities of current and future astronomical surveys.

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