Subsolar strange star mergers produce a lower post-merger-to-cutoff GW frequency ratio than neutron star mergers, cleanly separating the two classes across equations of state and mass ratios.
A large-scale magnetic field produced by a solar-like dynamo in binary neutron star mergers
5 Pith papers cite this work. Polarity classification is still indexing.
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abstract
The merger of neutron stars drives a relativistic jet which can be observed as a short gamma-ray burst. A strong large-scale magnetic field is necessary to launch the relativistic jet. However, the magnetohydrodynamical mechanism to build up this magnetic field remains uncertain. Here we show that the $\alpha\Omega$ dynamo mechanism driven by the magnetorotational instability builds up the large-scale magnetic field inside the long-lived binary neutron star merger remnant by performing an {\it ab initio} super-high resolution neutrino-radiation magnetohydrodynamics merger simulation in full general relativity. As a result, the magnetic field induces the Poynting-flux dominated relativistic outflow with the luminosity $\sim 10^{51}$\,erg/s and magnetically-driven post-merger mass ejection with the mass $\sim 0.1M_\odot$. Therefore, the magnetar scenario in binary neutron star mergers is possible. These can be the engines of short-hard gamma-ray bursts and very bright kilonovae. Therefore, this scenario is testable in future observation.
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High-resolution GR neutrino-radiation MHD simulation of 1.35-1.35 Msun BNS merger shows KHI-driven B-field amplification to magnetar levels (~10^50 erg, factor >=316) in 3 ms post-merger.
Improved Monte Carlo neutrino transport in BNS merger simulations that includes inelastic electron scattering and refined pair processes produces lower heavy-lepton neutrino energies/luminosities and 50% higher ejecta mass.
Analytical expressions for ALP-photon conversion in transient compact stars yield an updated bound g_aγ < 5×10^{-12} GeV^{-1} for m_a ≲ 10^{-9} eV from SN 1987A, plus sensitivity forecasts for future Galactic SN and NSM observations.
A grid-based multi-grid Poisson solver is implemented in numerical relativity, tested on puncture black holes and neutron stars, and used in a neutrino-radiation hydrodynamics simulation of 9 solar mass star collapse up to core bounce with high conservation accuracy.
citing papers explorer
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Subsolar-mass binary mergers of strange stars and neutron stars: gravitational waves and ejecta
Subsolar strange star mergers produce a lower post-merger-to-cutoff GW frequency ratio than neutron star mergers, cleanly separating the two classes across equations of state and mass ratios.
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A magnetar formation in binary neutron star merger
High-resolution GR neutrino-radiation MHD simulation of 1.35-1.35 Msun BNS merger shows KHI-driven B-field amplification to magnetar levels (~10^50 erg, factor >=316) in 3 ms post-merger.
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Impact of neutrino-electron scattering and an improved treatment of pair processes on binary neutron star mergers
Improved Monte Carlo neutrino transport in BNS merger simulations that includes inelastic electron scattering and refined pair processes produces lower heavy-lepton neutrino energies/luminosities and 50% higher ejecta mass.
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Axion-photon conversion in transient compact stars: Systematics, constraints, and opportunities
Analytical expressions for ALP-photon conversion in transient compact stars yield an updated bound g_aγ < 5×10^{-12} GeV^{-1} for m_a ≲ 10^{-9} eV from SN 1987A, plus sensitivity forecasts for future Galactic SN and NSM observations.
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Implementation of multi-grid Poisson solver in numerical relativity and its application to gravitational collapse of massive star
A grid-based multi-grid Poisson solver is implemented in numerical relativity, tested on puncture black holes and neutron stars, and used in a neutrino-radiation hydrodynamics simulation of 9 solar mass star collapse up to core bounce with high conservation accuracy.