NS-UNO: Neutron Star EoS Inference from an Unconstrained Number of Observations
nucl-th, astro-ph.HE, astro-ph.IM, hep-ph
Submitted: 2026-08-31
Updated: 2026-08-31
Terminology
Sources
- Neutron stars and the dense matter equation of state: from microscopic theory to macroscopic observations
- Properties of the binary neutron star merger GW170817
- GWTC-5.0: An Introduction to Version 5.0 of the Gravitational-Wave Transient Catalog
- Refined Mass and Geometric Measurements of the High-Mass PSR J0740+6620
- Markov Chain Monte Carlo Methods for Bayesian Data Analysis in Astronomy
- Cosmic Explorer: The U.S. Contribution to Gravitational-Wave Astronomy beyond LIGO
- Real-time gravitational-wave inference for binary neutron stars using machine learning
- Amortized Simulation-Based Inference of Relativistic Mean-Field Couplings for Neutron-Star Equations of State
- Neutron Star Equation of State via Physics Informed Neural Network
- A Partially Supervised Latent-Space Variational Autoencoder for Generating Neutron Star Equations of State
- Uncertainty quantification in the machine-learning inference from neutron star probability distribution to the equation of state
- Deep Sets
- Learning Likelihoods with Conditional Normalizing Flows
- Composition and thermodynamics of nuclear matter with light clusters
- Core-collapse supernova equations of state based on neutron star observations
- A New Parameterization for the Lagrangian Density of Relativistic Mean Field Theory
- Fast and Accurate Deep Network Learning by Exponential Linear Units (ELUs)
- Adam: A Method for Stochastic Optimization
Related papers
- BRST quantization for the restoration of broken symmetries: a pedagogical example
- FUSION: a skill-based research agent for publicly obtainable nuclear-physics codes
- Sensitivity of Neutron Star Observables to Transition Density in Hybrid Equation-of-State Models
- Exterior complex scaling enables physics-informed neural networks for quantum scattering
- Microscopic Insights into the Quarkyonic Hadron--Quark Crossover: Lessons from Ultracold Fermi Gases
- An Effective Upper Bound on the Pressure-to-Energy Density Ratio in Neutron Stars