Neutron-star physics
The Neutron-Star Equation of State
The still-uncertain relationship between pressure and density inside a neutron star, which decides how compressible its ultra-dense matter is and therefore the star's radius and maximum mass. Pinning it down — from radius measurements by NICER, from massive pulsars, and from the tidal signature in neutron-star mergers — is a central goal of modern astrophysics.
Highlights
- ›The uncertain physics that sets a neutron star's size
Classes, physics & objects
Across compact objects
Knowledge connections
- Associated withNeutron Degeneracy Pressure
- Associated withNeutron Star
- Associated withNeutron Degeneracy Pressure
- Associated withBinary Neutron Star Merger
- Associated withPSR J0740+6620
- Associated withPulsar Glitch
- Associated withPSR J0740+6620
Sources
The primary and reference sources this topic draws on.
- NASANational Aeronautics and Space Administration
Mission data, planetary science, space telescopes, and public-domain imagery.
Most NASA-produced imagery is in the public domain; individual items are checked for usage terms before publication.