Effect of magnetic field quantization on the shallow acceptor spectrum in strained Ge/GeSi heterostructures

2002 ◽  
Vol 66 (15) ◽  
Author(s):  
V. Ya. Aleshkin ◽  
V. I. Gavrilenko ◽  
D. B. Veksler ◽  
L. Reggiani
Keyword(s):  
Magnetic Field ◽  
Shallow Acceptor ◽  
Field Quantization

The effect of magnetic field quantization on the propagation of shock waves in quantum plasmas

2019 ◽  
Vol 26 (5) ◽  
pp. 052105 ◽  
Author(s):  
S. Hussain ◽  
Hafeez Ur-Rehman ◽  
S. Mahmood
Keyword(s):  
Magnetic Field ◽  
Shock Waves ◽  
Quantum Plasmas ◽  
Field Quantization

Theoretical calculations of shallow acceptor states in GaAs/AlxGa1−xAs quantum wells in the presence of an external magnetic field

1994 ◽  
Vol 50 (4) ◽  
pp. 2393-2398 ◽  
Author(s):  
Q. X. Zhao ◽  
P. O. Holtz ◽  
Alfredo Pasquarello ◽  
B. Monemar ◽  
M. Willander
Keyword(s):  
Magnetic Field ◽  
External Magnetic Field ◽  
Quantum Wells ◽  
Theoretical Calculations ◽  
Shallow Acceptor

The magnetic field quantization in pulsar

2020 ◽  
Author(s):  
Chaudhary Rozina ◽  
Tsintsadze LevanNodar ◽  
Nodar Tsintsadze
Keyword(s):  
Magnetic Field ◽  
Neutron Star ◽  
Magnetic Pressure ◽  
Wave Number ◽  
Cyclotron Energy ◽  
Parallel Propagation ◽  
Quantum Electron ◽  
Jeans Instability ◽  
Exotic Physics ◽  
Field Quantization

<p>Magnetic field quantization is an important issue for degenerate environments such as neutron star, radio pulsars and magnetars etc., due to the fact that these stars have magnetic field even more than the quantum critical field strength of the order of 4.4×10¹³G, accordingly the cyclotron energy may be equal or even much more than the Fermi energy of degenerate particles. We shall formulate here the exotic physics of strongly magnetized neutron star. The effect of quantized anisotropic magnetic pressure, arising due to a strong magnetic field is studied on the growth rate of Jeans instability of quantum electron–ion and classical dusty plasma.  Here we shall formulate the dispersion equations to govern the propagation of the gravitational waves both in perpendicular and parallel directions to the magnetic field, respectively.  We will depict here that the quantized magnetic field will result in Jeans anisotropic instability such that for perpendicular propagation, the quantized magnetic pressure will stabilize Jeans instability, whereas for the parallel propagation the plasma become more unstable.  We also intend to calculate the corresponding Jeans wave number in the absence of tunneling. The Madelung term leads to the inhomogeneity of the plasma medium. Numerical results are presented to show the effect of the anisotropic magnetic pressure on the Jeans instability.</p>

OPTICAL PROPERTIES OF ACCEPTORS IN SEMIMAGNETIC QUANTUM WELL SYSTEMS

2002 ◽  
Vol 16 (25) ◽  
pp. 3737-3757 ◽  
Author(s):  
Sr. GERARDIN JAYAM ◽  
K. NAVANEETHAKRISHNAN
Keyword(s):  
Magnetic Field ◽  
Magnetic Fields ◽  
Quantum Well ◽  
Cross Sections ◽  
Empirical Relationship ◽  
Phonon Interaction ◽  
Shallow Acceptor ◽  
Electron Phonon Interaction ◽  
The Magnetic Field ◽  
Confined Phonons

The binding energy of a shallow acceptor in an isolated quantum well of the CdTe / Cd 1-x Mn x Te system has been investigated in an external magnetic field, assuming an empirical relationship between the barrier height and the magnetic field. Photoionization cross-sections for different magnetic fields have been estimated. Taking into account the confined phonons in the electron-phonon interaction, carrier capture times for various magnetic fields and different hydrostatic pressures have been computed. The results obtained are discussed in the light of the existing literature.

Magnetic field quantization in pulsars

2020 ◽  
Vol 86 (2) ◽  
Author(s):  
Ch. Rozina ◽  
N. L. Tsintsadze ◽  
L. N. Tsintsadze
Keyword(s):  
Magnetic Field ◽  
Neutron Stars ◽  
Wave Solution ◽  
Solitary Wave Solution ◽  
Phase Speed ◽  
Compact Objects ◽  
Neutron Density ◽  
Quantum Hydrodynamic Model ◽  
Cyclotron Energy ◽  
Field Quantization

Magnetic field quantization is an important issue for degenerate environments such as neutron stars, radio pulsars and magnetars etc., due to the fact that these stars have a magnetic field higher than the quantum critical field strength of the order of $4.4\times 10^{13}~\text{G}$ , accordingly, the cyclotron energy may be equal to or even much more than the Fermi energy of degenerate particles. We shall formulate here the exotic physics of strongly magnetized neutron stars, known as pulsars, specifically focusing on the outcomes of the quantized magnetic pressure. In this scenario, while following the modified quantum hydrodynamic model, we shall investigate both linear and nonlinear fast magnetosonic waves in a strongly magnetized, weakly ionized degenerate plasma consisting of neutrons and an electron–ion plasma in the atmosphere of a pulsar. Here, linear analysis depicts that sufficiently long, fast magnetosonic waves may exist in a weakly dispersive pulsar having finite phase speed at cutoff. To investigate one-dimensional nonlinear fast magnetosonic waves, a neutron density expression as a function of both the electron magnetic and neutron degenerate pressures, is derived with the aid of Riemann’s wave solution. Consequently, a modified Korteweg–de Vries equation is derived, having a rarefractive solitary wave solution. It is found that the basic properties such as amplitude, width and phase speed of the fast magnetoacoustic waves are significantly altered by the electron magnetic and the neutron degenerate pressures. The results of this theoretical investigation may be useful for understanding the formation and features of the solitary structures in astrophysical compact objects such as pulsars, magnetars and white dwarfs etc.

Magnetic-field strengths from optical polarization data

1967 ◽  
Vol 31 ◽  
pp. 381-383
Author(s):  
J. M. Greenberg
Keyword(s):  
Magnetic Field ◽  
Optical Polarization ◽  
Polarization Data ◽  
Term Model ◽  
Source Of Information ◽  
Field Strengths

Van de Hulst (Paper 64, Table 1) has marked optical polarization as a questionable or marginal source of information concerning magnetic field strengths. Rather than arguing about this–I should rate this method asq+-, or quarrelling about the term ‘model-sensitive results’, I wish to stress the historical point that as recently as two years ago there were still some who questioned that optical polarization was definitely due to magnetically-oriented interstellar particles.

Observing the galactic magnetic field

1967 ◽  
Vol 31 ◽  
pp. 375-380
Author(s):  
H. C. van de Hulst
Keyword(s):  
Magnetic Field ◽  
Fair Agreement ◽  
Solar Neighbourhood ◽  
Galactic Magnetic Field ◽  
The Magnetic Field

Various methods of observing the galactic magnetic field are reviewed, and their results summarized. There is fair agreement about the direction of the magnetic field in the solar neighbourhood:l= 50° to 80°; the strength of the field in the disk is of the order of 10-5gauss.

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