MHD waves with Landau diamagnetic pressure and Pauli paramagnetizim in degenerate plasmas

Abstract

Magnetosonic waves are studied in the presence of degenerate pressure due to Landau diamagnetic levels and Pauli spin magnetization with strong magnetic field in quantum degenerate electron-ion plasma. A linear dispersion relation of low frequency propagation wave in the direction of magnetic field is derived that strongly depends on the magnetic field while in classical regime this field has no such a role. In the presence of quantization of orbital motion and spin magnetization, new propagation modes of quantum plasmas are also explored. It is noted that quantum acoustic velocity and spin magnetization energy affect the Alfven mode propagation. The quantum effects are incorporated through the Bohm potential, Landau pressure due to Landau quantization of magnetic field and magnetization energy due to spin effect. The current model in the context of Landau diamagnetic pressure along with spin magnetization is sufficient for studying the astrophysical plasma environment existing in the compact systems e.g., white dwarfs and neutron stars.and while the field of interior core of NS can reach ;10 11 Tesla or even may be higher [9][10][11]. Further this field may be increased by a factor 10 3 ∼10 4 due to the rotational movement of stars RECEIVED

The impact of quantized magnetic pressure on the stimulated Brillouin scattering of electromagnetic waves

“…To see more clearly the impact of SSH field on the dispersive characteristics of the MSBS instability of EMWs, we analyze Equations ( 26), ( 28), (30) numerically. For this purpose, we choose the typical plasma parameters in the atmosphere of neutron stars in cgs system of units: H 0 ; 10 10 − 10 12 G (in the surface crust of neutron star NS) [68], n e0 = 3 × 10 24 cm −3 c = 2.99 × 10 10 cms −1 , m e = 9.1 × 10 −28 g, m i = 1.67 × 10 −24 g, e = 4.8 × 10 −10 stat coloumb, ÿ = 1.05 × 10 −27 cm 2 gs −1 and k B = 1.3807 × 10 −16 cm 2 gs −2 K −1 . The prerequisite condition for the magnetic field quantization to occur i.e, w e > ce F e  is found to be satisfied at H 0 ∼ 2 × 10 10 G. For the choice of the electron density used here, the cutoff frequency of EM waves turns out to be ω = 9.7 × 10 16 Hz, so the present model is valid for the propagation of EM waves having frequencies > 9.7 × 10 16 Hz i.e.…”

Synchrotron emitting Komissarov torus with magnetic polarization around Kerr black holes

“…Magnetic properties of plasmas have been studied in quantum collisional and collisionless plasmas (A. V. Latyshev & A. Yushkanov 2017) or in the propagation of waves quantum plasmas (A. Safdar et al 2020; N. Sadiq & M. Ahmad 2019) considering the Landau diamagnetism and Pauli paramagnetism applicable astrophysical scenarios like neutron stars, extragalactic jets or in auroral forms, where the acceleration of electrons is generated by magnetic fields. Expression for magnetic susceptibility in these cases is similar to equation (1) where the relation between 𝐻 and 𝑇 is equivalent to equation ( 5).…”

Magnetorotational instability in dense electron–positron–ion plasmas

“…Beyond these limitations, Misra et al 30 studied the influence of the intrinsic spin of electrons on the propagation of circularly polarized waves in a magnetized plasma. Safdar et al 31 investigated magnetosonic waves in the presence of degenerate pressure due to Landau diamagnetic levels and Pauli spin magnetization and explored a new propagation mode. A model for dense degenerate plasmas that incorporates electron spin 32 , magnetosonic solitary waves 33 , effects of the spin on the EM wave modes in magnetized plasmas 34 , basic properties of magnetosonic waves in a magnetorotating spin quantum plasma 35 and instability of Terahertz (THz) plasma waves 36 in quantum field effect transistors (FETs) with the spin effects are extensively studied and were found to play major roles in specifying the nature, structures and features of astrophysical (neutron stars and white dwarfs) and laboratory (semiconductor) plasmas.…”