Causal convolutional neural networks reconstruct neutron star observables for static, Keplerian, and rotating configurations in about 50 milliseconds per equation of state, compared to 30 minutes with traditional RNS calculations.
A Radio Pulsar Spinning at 716 Hz
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The (axial-)vector meson extended linear sigma model yields an equation of state for quark matter that satisfies astrophysical constraints on compact star masses and radii.
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Reconstruction of fast-rotating neutron star observables with the neural network
Causal convolutional neural networks reconstruct neutron star observables for static, Keplerian, and rotating configurations in about 50 milliseconds per equation of state, compared to 30 minutes with traditional RNS calculations.
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Compact star properties from an extended linear sigma model
The (axial-)vector meson extended linear sigma model yields an equation of state for quark matter that satisfies astrophysical constraints on compact star masses and radii.