The Diamagnetic Phase Transition of Dense Electron Gas: Astrophysical Applications

Wang, Zhaojun; Zhu, Chunhua; Wu, Baoshan

doi:10.1088/1538-3873/128/968/104201

Cited by 9 publications

(10 citation statements)

References 67 publications

(110 reference statements)

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“…They conclude that magnetic domains can be formed in the crust and core of magnetars. Moreover, as it was mentioned by Wang et al (2016), neutron stars are ideal astrophysical laboratories to test the de Haas-van Alphen effect (De Haas & Van Alphen 1930), in which the magnetic susceptibility oscilates as the magnetic field is increased, and also to explain the diamagnetic phase transition, which is associated with magnetic domain formation. On the other hand, Kiuchi et al (2015) found a magnetic field amplification of ≈ 10 3 times the initial magnetic field due to the KHI in a binary neutron star merger.…”

Section: Introductionmentioning

confidence: 99%

On the linear and non-linear evolution of the relativistic MHD Kelvin–Helmholtz instability in a magnetically polarized fluid

Pimentel

Lora-Clavijo

2019

Monthly Notices of the Royal Astronomical Society

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The origin and strength of the magnetic field in some systems like active galactic nuclei or gamma-ray bursts is still an open question in astrophysics. A possible mechanism to explain the magnetic field amplification is the Kelvin-Helmholtz instability, since it is able to transform the kinetic energy in a shear flow into magnetic energy. Through the present work, we investigate the linear and non linear effects produced by the magnetic susceptibility in the development of the Kelvin-Helmholtz instability in a relativistic plasma. The system under study consists of a plane interface separating two uniform fluids that move with opposite velocities. The magnetic field in the system is parallel to the flows and the susceptibility is assumed to be homogeneous, constant in time, and equal in both fluids. In particular, we analyze the instability in three different cases, when the fluids are diamagnetic, paramagnetic, and when the susceptibility is zero. We compute the dispersion relation in the linear regime and found that the interface between diamagnetic fluids is more stable than between paramagnetic ones. We check the analytical results with numerical simulations, and explore the effect of the magnetic polarization in the non linear regime. We find that the magnetic field is more amplified in paramagnetic fluids than in diamagnetic ones. Surprisingly, the effect of the susceptibility in the amplification is stronger when the magnetization parameter is smaller. The results of our work make this instability a more efficient and effective amplification mechanism of seed magnetic fields when considering the susceptibility of matter.

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Section: Introductionmentioning

confidence: 99%

On the linear and non-linear evolution of the relativistic MHD Kelvin–Helmholtz instability in a magnetically polarized fluid

Pimentel

Lora-Clavijo

2019

Monthly Notices of the Royal Astronomical Society

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“…Distinguishing from rotation powered, the activity is powered by magnetic field with energy deposited in domain structure and the shear deformation of solid crust (if the depinning transition induces brittle fracture). Available magnetic free energy [53] may reach up to 10 38 (B/B Q ) 4 erg only in domain structure. The seismic waves however cannot propagate directly to the surface but by many reflections [61] between the surface and evanescent zone (where the magnetic stress begins to dominate the crust stress).…”

Section: Summary and Discussionmentioning

confidence: 99%

“…the differential magnetic susceptibility χ m = ∂(4πM )/∂H > 1, homogeneous magnetized state transforms into Condon domain structure [52]. The instability condition and feature of magnetic domains and domain walls were studied in more detail in [39] and [53].…”

Section: B Magnetic Oscillatory In Magnetized Neutron Starmentioning

confidence: 99%

Magnetic-oscillation mechanism for understanding periodic or quasi-periodic modulation of the timing residuals from pulsars

Wang¹,

C²,

Li³

et al. 2018

Preprint

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Highly precise pulsar timing is very important for understanding the nature of neutron stars and the implied physics, even being used to detect directly gravitational waves. Unfortunately, the accuracy of the pulsar timing is seriously affected by the spin-down irregularities, such as spin fluctuations with a manifestation of low frequency structures (the so-called red noise processes), and various activities of magnetospheres. Except from the random timing noise, significant periodic or quasi-periodic components could also be found in some timing residuals of pulsars, indicating the presence of unmodelled deterministic effects. The physical origins of these effects still remain unexplained. In this paper, we suggest a new mechanism involving the de Haas-van Alphen magnetic oscillation, which could trigger the observed low frequency structures. We find that the proposed magnetic oscillation period is about 1-10 2 yr, which is about 10 −4 times as long as the classical characteristic time scale of interior magnetic field evolution for a normal neutron star. Due to the magnetic oscillation, we estimate both the braking index range between 10 −5 and 10 5 and the residuals range between 4 to 906 ms for some specific samples of quasi-periodic pulsars. Those are consistent with the pulsar timing observations. Nonlinear phenomena of de Haas-van Alphen effect and the Condon domain structure are considered. Avalanche-like magnetized process of domain wall motion (rapidly magnetic energy release) could associated with some special emitting manifestations of neuron star radiation.

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“…Indeed, Suh & Mathews (2010) consider the possibility that the soft gamma-ray repeaters and the anomalous X-ray pulsars might be observational evidence for a diamagnetic phase transition that results in a domain formation. Furthermore, as mentioned by Wang et al (2016), neutron stars are also important for testing the Haas-van Alphen effect in which the magnetic susceptibility oscillates when the applied magnetic field is increased (De Haas & Van Alphen 1930).…”

Section: Introductionmentioning

confidence: 99%

Analytic solution of a magnetized tori with magnetic polarization around Kerr black holes

Pimentel

Lora-Clavijo

González

2018

A&A

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We present the first family of magnetically polarized equilibrium tori around a Kerr black hole. The models were obtained in the test fluid approximation by assuming that the tori is a linear media, making it is possible to characterize the magnetic polarization of the fluid through the magnetic susceptibility χ m . The magnetohydrodynamic (MHD) structure of the models was solved by following the Komissarov approach, but with the aim of including the magnetic polarization of the fluid, the integrability condition for the magnetic counterpart was modified. We build two kinds of magnetized tori depending on whether the magnetic susceptibility is constant in space or not. In the models with constant χ m , we find that the paramagnetic tori (χ m > 0) are more dense and less magnetized than the diamagnetic ones (χ m < 0) in the region between the inner edge, r in , and the center of the disk, r c ; however, we find the opposite behavior for r > r c . Now, in the models with non-constant χ m , the tori become more magnetized than the Komissarov solution in the region where ∂χ m /∂r < 0, and less magnetized when ∂χ m /∂r > 0. Nevertheless, it is worth mentioning that in all solutions presented in this paper the magnetic pressure is greater than the hydrodynamic pressure. These new equilibrium tori can be useful for studying the accretion of a magnetic media onto a rotating black hole.

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The Diamagnetic Phase Transition of Dense Electron Gas: Astrophysical Applications

Cited by 9 publications

References 67 publications

On the linear and non-linear evolution of the relativistic MHD Kelvin–Helmholtz instability in a magnetically polarized fluid

On the linear and non-linear evolution of the relativistic MHD Kelvin–Helmholtz instability in a magnetically polarized fluid

Magnetic-oscillation mechanism for understanding periodic or quasi-periodic modulation of the timing residuals from pulsars

Analytic solution of a magnetized tori with magnetic polarization around Kerr black holes

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