Neutron Star Heating Constraints on Wave-Function Collapse Models.

Area of Science:

• Quantum mechanics
• Astrophysics
• Cosmology

Background:

• Spontaneous wave-function collapse models aim to resolve the quantum measurement problem.
• These models suppress macroscopic superpositions while preserving quantum phenomena at microscopic scales.
• A key prediction is the spontaneous heating of massive objects.

Purpose of the Study:

• To calculate the heating rate and equilibrium temperature induced by collapse models in astrophysical objects.
• To apply these calculations to neutron stars, the densest baryonic matter.
• To derive bounds on collapse model parameters using neutron star observations.

Main Methods:

• Theoretical calculation of collapse-induced heating rates.
• Determination of equilibrium temperatures for massive objects.
• Application of models to neutron star properties and observational data.

Main Results:

• Collapse model parameters directly correlate with heating rates; stronger parameters lead to greater heating.
• Derived competitive bounds on spontaneous collapse model parameters using neutron star data.
• Proposed speculative bounds based on current and future astronomical survey capabilities.

Conclusions:

• Neutron star observations offer a viable method for constraining spontaneous wave-function collapse models.
• The study provides a framework for using astrophysical data to test fundamental physics.
• Future astronomical observations can further refine or challenge these quantum gravity models.