Oscillations of highly magnetized non-rotating neutron stars

Leung, Man Yin; Yip, Anson Ka Long; Cheong, Patrick Chi-Kit; Li, Tjonnie G. F.

doi:10.1038/s42005-022-01112-w

Cited by 9 publications

(4 citation statements)

References 80 publications

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“…More details of the simulation set-ups can be found in Leung et al [7] and Yip et al [8,9]. Here, we briefly highlight the important features of the set-ups.…”

Section: Methodsmentioning

confidence: 99%

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Dynamics and gravitational wave signatures of highly magnetized compact stars

Yip¹

2023

Proceedings of 38th International Cosmic Ray Conference — PoS(ICRC2023)

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Strong magnetic fields make neutron stars potential sources of detectable electromagnetic and gravitational-wave signals. Hence, inferring these magnetic fields is critical to understand the emissions of neutron stars. However, the interior magnetic field configuration remains ambiguous due to the lack of direct observational evidence. Here, for the first time, we show that the internal magnetic field strength along with the composition of a neutron star can be directly constrained by detecting the gravitational waves from the phase-transition-induced collapse of a magnetized neutron star. In particular, we study the effects of magnetic fields and phase-transition-induced collapses on the dynamics, oscillation modes, and gravitational-wave signatures of compact stars through dynamical simulations. Hence, this work has demonstrated that much information inside neutron stars could be extracted by measuring the oscillation modes from the gravitational waves emitted by the stars.

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“…More details of the simulation set-ups can be found in Leung et al [7] and Yip et al [8,9]. Here, we briefly highlight the important features of the set-ups.…”

Section: Methodsmentioning

confidence: 99%

“…In this proceeding, we present our recent works on simulating highly magnetized compact stars [7][8][9]. Specifically, we first discuss the pure magnetic effect (without considering any phase transition effect) on the oscillation modes of magnetized neutron stars with maximum magnetic field strength B max ∼ 10 15−17 G .…”

Section: Introductionmentioning

confidence: 99%

Dynamics and gravitational wave signatures of highly magnetized compact stars

Yip¹

2023

Proceedings of 38th International Cosmic Ray Conference — PoS(ICRC2023)

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“…In Paper I (Cheong et al 2023), we mentioned the formulations of the general-relativistic multifrequency radiation transport module within the General-relativistic multigrid numerical (Gmunu) code (Cheong et al 2020(Cheong et al , 2021(Cheong et al , 2022, which has been widely used in multiple applications (Ng et al 2021;Leung et al 2022;Yip et al 2023). The module is based on the two-moment general-relativistic multifrequency radiative transfer scheme (Thorne 1981;Shibata et al 2011;Cardall et al 2013a).…”

Section: Introductionmentioning

confidence: 99%

General-relativistic Radiation Transport Scheme in Gmunu. II. Implementation of Novel Microphysical Library for Neutrino Radiation—Weakhub

Ng,

Cheong 張,

Lam

et al. 2024

ApJS

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We introduce Weakhub, a novel neutrino microphysics library that provides opacities and kernels beyond conventional interactions used in the literature. This library includes neutrino–matter, neutrino–neutrino interactions and plasma process, along with corresponding weak and strong corrections. A full kinematics approach is adopted for the calculations of β-processes, incorporating various weak corrections and medium modifications due to the nuclear equation of state. Calculations of plasma processes, electron neutrino–antineutrino annihilation, and nuclear de-excitation are also included. We also present the detailed derivations of weak interactions and the coupling to the two-moment based general-relativistic multigroup radiation transport in the general-relativistic multigrid numerical (Gmunu) code. We compare the neutrino opacity spectra for all interactions and estimate their contributions at hydrodynamical points in core-collapse supernovae and binary neutron star (BNS) postmerger remnants, and predict the effects of improved opacities in comparison to conventional ones for a BNS postmerger at a specific hydrodynamical point. We test the implementation of the conventional set of interactions by comparing it to an open-source neutrino library NuLib in a core-collapse supernova simulation. We demonstrate good agreement with discrepancies of less than ∼10% in luminosity for all neutrino species, while also highlighting the reasons contributing to the differences. To compare the advanced interactions to the conventional set in core-collapse supernova modeling, we perform simulations to analyze their impacts on neutrino signatures, hydrodynamical behaviors, and shock dynamics, showing significant deviations.

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“…The approaches of using MHD modeling in the transport of SEPs allow for a more comprehensive representation of the underlying physical processes and improve the fidelity of the simulation results to observations. MHD can be used to simulate the plasma environment in various situations, such as the plasma environment in astrophysics (e.g., Kim & Ostriker 2002;Ruszkowski et al 2011;Leung et al 2022), solar atmosphere (e.g., Linker et al 1999;Jiang et al 2016), the heliospheric space physics environment (e.g., Usmanov et al 2000;Shen et al 2018), the Earth space environment (e.g., Wu et al 1981;Janhunen et al 2012), nuclear fusion experiments (tokamak; e.g., Tani et al 1992;Connor et al 1998), spheromak experiments to study magnetic reconnection (e.g., Schnack et al 1998;Lukin et al 2001), and so on. In the past, significant efforts have been made to numerically solve MHD equations.…”

Section: Introductionmentioning

confidence: 99%

Modeling the Transport of Solar Energetic Particles in a Corotating Interaction Region

Zhong,

Qin,

2024

ApJ

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We present a new three-dimensional (3D) magnetohydrodynamic (MHD) model and a new 3D energetic particle transport (EPT) model. The 3D MHD model numerically solves the ideal MHD equations using the relaxing total variation diminishing scheme. In the 3D MHD simulations, we use simple boundary conditions with a high-speed flow, and we can clearly identify a corotating interaction region (CIR) with the characteristics of forward shock and reverse shock. The 3D EPT model solves the Fokker–Planck transport equation for the solar energetic particles (SEPs) using backward stochastic processes, with the magnetic field and solar wind velocity field from MHD results. For comparison, the 3D EPT model results with Parker fields are also obtained. We investigate the transport of SEPs with particle sources and observers in different positions in MHD fields with a CIR, and we compare the results with those in the Parker fields. Our simulation results show that the compression region with local enhancement of the magnetic field, i.e., CIR, can act as a barrier to scatter energetic particles back, and particles can struggle to diffuse through the strong magnetic field regions. Usually, a normal anisotropy profile is commonly present in SEP simulation results with Parker fields, and it is also typically present in that with MHD fields. However, because of the compression region of the magnetic field, energetic particles may exhibit anomalous anisotropy. This result may be used to replicate the spacecraft observation phenomena of the anomalous anisotropy.

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Oscillations of highly magnetized non-rotating neutron stars

Cited by 9 publications

References 80 publications

Dynamics and gravitational wave signatures of highly magnetized compact stars

Dynamics and gravitational wave signatures of highly magnetized compact stars

General-relativistic Radiation Transport Scheme in Gmunu. II. Implementation of Novel Microphysical Library for Neutrino Radiation—Weakhub

Modeling the Transport of Solar Energetic Particles in a Corotating Interaction Region

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