Gravitational Instability Analysis in Multi-Ion Dense Quantum Magnetoplasma
A. Mushtaq, Sajad Ali, Zahida Ehsan
备注：
We submitted this article to a couple of journals but it got rejected. Because this model is fundamentally wrong. So we request for the withdrawal of this article
Electrostatic Gravitational or Rayleigh-Taylor (RT) instability in an inhomogeneous magnetized multi-ions plasma with some fraction of quantum mechanical electrons. The effect of Bohm potential, temperature degeneracy and magnetic field are carried out. A generalized dispersion relation is deduced under the drift approximation. The presence of negative ions with their different streaming velocities make the dispersion relation a cubic equation. Different roots of both real and imaginary parts of the RT mode are studied by using the Cardano method of solving the cubic equation. The growth rates of RT instability are examined analytically and numerically. It is shown that the basic features of these waves are significantly modified by the positive and negative ions drift speed as well as by the magnetic field and density. Relevance of the work regarding to dense astrophysical plasmas is pointed out.
Generation of wakefields by whistlers in spin quantum magnetoplasmas
本文报道了在磁化自旋量子等离子体中，由哨声波引起的经典有质动力和自旋诱导有质动力（分别为CPF和SPF）对静电尾场的激发。哨声和尾流场的非线性动力学被证明是由一组耦合的非线性薛定谔（NLS）和驱动Boussinesq方程。研究发现，与玻姆势相关的量子力引入了两个特征尺度，导致强磁化稠密等离子体（具有典型的磁场强度$B_{0}\gtrsim10^{9}$ T和粒子密度$n_{0}\gtrsim10^{36}$ m $^{-3}$）中多个尾波场的激发，其中SPF强于CPF.在其他的状态下，即$B_{0}\lesssim10^{8}$ T和$\ n_{0}\lesssim10^{35}$ m $^{-3}$，其中SPF与CPF相当，等离子体尾场也可以用一个特征长度尺度自洽地激发。数值结果表明，量子隧穿效应使尾波场振幅增大，而外加磁场使尾波场振幅减小。在适当的条件下，尾场可以在多个等离子体波长上保持高相干性，从而将电子加速到极高的能量。结果可能是有用的粒子加速在短尺度，即在纳米和微米尺度，在磁化稠密等离子体中的驱动器是哨声波，而不是激光或粒子束。
Modulational instability and nonlinear evolution of two-dimensional electrostatic wave packets in ultra-relativistic degenerate dense plasmas
研究了超相对论（UR）简并稠密电子-离子等离子体中静电波包的非线性传播，其动力学过程由非局域二维非线性类薛定谔方程控制.然后利用耦合方程组研究了均匀波列对多维形式的微扰的调制不稳定性。得到了MI的条件，并证明了与简并电子UR压力相关的无量纲参数$β\proptoλ_C n_0^{1/3}$（$λ_C$是约化康普顿波长，$n_0$是粒子数密度）使$n_{0}\sim10^{30}$ cm $^{-3}$处的稳定（不稳定）区域向更高密度处的不稳定（稳定）区域（即$n_{0}\gtrsim7\times10^{33}$）移动.研究还发现，$n_{0}$的值越高，调制波数越低时截止MI的增长率越低。此外，数值研究了波包的动力学演化。我们表明，它们要么分散或爆破在有限的时间内，当波的作用是低于或高于阈值。这些结果对于理解UR简并致密等离子体中调制波包的性质及其多维演化，例如白矮星{和/或}前超新星恒星内部的调制波包的性质具有重要意义.
