REVIEW 8 cited by
Emergence of microphysical bulk viscosity in binary neutron star post-merger dynamics
Not yet reviewed by Pith; the record is open.
This paper has not been read by Pith yet. Machine review is queued; the pith claim, tier, and objections will appear here once it completes.
SPECIMEN: schema-true, not a live event
T0 review · schema-true
One-sentence machine reading of the paper's core claim.
pith:XXXXXXXX · record.json · timestamp
abstract
In nuclear matter in isolated neutron stars, the flavor content (e.g., proton fraction) is subject to weak interactions, establishing flavor ($\beta$-)equilibrium. However, there can be deviations from this equilibrium during the merger of two neutron stars. We study the resulting out-of-equilibrium dynamics during the collision by incorporating direct and modified Urca processes (in the neutrino-transparent regime) into general-relativistic hydrodynamics simulations with a simplified neutrino transport scheme. We demonstrate how weak-interaction-driven bulk viscosity in post-merger simulations can emerge and assess the bulk viscous dynamics of the resulting flow. We further place limits on the impact on the post-merger gravitational wave strain. Our results show that weak-interaction-driven bulk viscosity can potentially lead to a phase shift of the post-merger gravitational wave spectrum, although the effect is currently on the same level as the numerical errors of our simulation.
Forward citations
Cited by 8 Pith papers
-
Neutrino absorption in two-flavor color-superconducting quark matter
In 2SC quark matter, neutrino absorption is dominated by strange-quark capture at low temperature, and a degenerate neutrino gas at electron lepton fraction 0.1 has a mean free path of meters or less.
-
Superradiant amplification by rotating viscous compact objects
Using causal BDNK hydrodynamics, the authors derive coupled gravitational-wave and viscous-mode equations for slowly rotating stars and find superradiant amplification at low frequencies.
-
Radial Oscillations of Viscous Stars
Viscosity damps neutron-star radial modes on ms timescales, shifts frequencies by up to ~1% at ζ∼10^30 g/cm/s, produces overdamped modes above ∼10^31, and cannot stabilize unstable stars in Eckart or BDNK theory.
-
Hydrodynamical transports in generic AdS Gauss-Bonnet-scalar Gravity
Analytic shear and bulk viscosity formulas are derived for a five-dimensional Einstein-Scalar-Maxwell-Gauss-Bonnet holographic model, with the shear viscosity cross-checked by Kubo methods.
-
Bulk viscosity and $n$-component fluids
A general framework for n-component bulk viscosity in second-order hydrodynamics, with transport coefficients expressed as matrix invariants and a Green's function that decomposes into n Israel-Stewart modes.
-
TTE-CAM: Self-Explainable Class Activation Maps for Pretrained Black-Box CNNs
A test-time convolution-head replacement converts pretrained CNNs into self-explainable models that keep black-box accuracy and produce faithful class activation maps.
-
Nuclear matter equation of state and astrophysics
A review of multimessenger constraints on the neutron-star equation of state, arguing composition remains undetermined and advocating a multidimensional EoS framework and the author-affiliated MUSES software.
-
The equation of state for neutron stars
A textbook-style review of the neutron-star equation of state covering the models, experimental and observational constraints, and open questions, with no new result claimed or derived.
Discussion (0). Sign in to comment.