Linked from

The 10 pages that link to Neutron-star equation of state, each with the reason it gives.

• Equation of stateBroader topic: It determines how predicted neutron-star masses and radii depend on dense-matter physics.

• PulsarRelated: Pulsar masses and rotation constrain the possible properties of ultradense matter.

• Multi-messenger astronomyRelated: Merger signals and subsequent radiation constrain the properties of ultra-dense matter.

• Binary pulsarRelated: Accurate binary mass measurements rule out equations of state unable to support observed stars.

• GW170817Related: GW170817 constrained this relation without uniquely determining the composition of dense matter.

• MagnetarRelated: Magnetar observations can constrain the properties of matter at densities beyond terrestrial experiments.

• Crab PulsarRelated: Crab glitches and spin evolution constrain models of matter under neutron-star conditions.

• Scorpius X-1Related: Accretion and timing studies of Scorpius X-1 help constrain models of neutron-star matter.

• X-ray pulsarRelated: Pulsar mass and radius measurements constrain the behavior of matter at extreme density.

• Radio-quiet neutron starRelated: Multiwavelength measurements of radio-quiet stars can constrain their sizes and internal matter.