# Neutron star heating constraints on wave-function collapse models

## TL;DR

This paper investigates how wave-function collapse models cause heating in neutron stars, deriving bounds on model parameters from astrophysical observations and proposing future observational constraints.

## Contribution

It calculates collapse-induced heating rates for neutron stars and derives new bounds on collapse model parameters from astrophysical data.

## Key findings

- Stronger collapse parameters lead to higher neutron star temperatures.
- Neutron star observations set competitive bounds on collapse models.
- Future surveys could tighten these bounds further.

## Abstract

Spontaneous wavefunction collapse models, like the 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. Here 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.