Quantum inertial Alfvén solitary waves: the effect of exchange-correlation and spin magnetization

Sadiq, Nauman; Ahmad, Masood

doi:10.1080/17455030.2020.1718243

Cited by 6 publications

(1 citation statement)

References 41 publications

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“…Similarly Marklund, Brodin and Garai in [36][37][38] have proposed the spin-1/ 2 quantum MHD (QMHD) models for MHD and oblique MHD waves. Linear and non linear propagation of kinetic Alfven and inertial Alfvén waves with effects of spin magnetization and exchangecorrelation potential have been investigated in [39,40]. Waves and instabilities in relativistic anisotropic magnetohydrodynamic plasma were examined by Patidar et al in [41].…”

Section: Introductionmentioning

confidence: 99%

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

Safdar¹,

Ahmad²,

Esmaeili³

et al. 2020

Phys. Scr.

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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

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