Phonons in a magnetized Coulomb crystal of ions with polarizable electron background

2017 ◽  
Vol 24 (11) ◽  
pp. 112704 ◽  
Author(s):  
D. A. Baiko ◽  
A. A. Kozhberov
Keyword(s):  
Coulomb Crystal

Sympathetic cooling in a multi-isotope Sr+Coulomb crystal

2010 ◽  
Author(s):  
S. Removille ◽  
Q. Glorieux ◽  
T. Coudreau ◽  
L. Guidoni ◽  
J.-P. Likforman ◽  
...  
Keyword(s):  
Sympathetic Cooling ◽  
Coulomb Crystal

Forces acting on a coulomb crystal of microparticles in plasma

1998 ◽  
Vol 39 (6) ◽  
pp. 825-831 ◽  
Author(s):  
I. V. Schweigert ◽  
V. A. Schweigert
Keyword(s):  
Coulomb Crystal

A comparative study between effects of shadowing potential and ODS on Coulomb crystal formation

2010 ◽  
Vol 77 (4) ◽  
pp. 547-557 ◽  
Author(s):  
SWATI BARUAH ◽  
NILAKSHI DAS
Keyword(s):  
Distribution Function ◽  
Comparative Study ◽  
Radial Distribution Function ◽  
Radial Distribution ◽  
Coupling Parameter ◽  
Dynamics Simulation ◽  
Crystal Formation ◽  
Coulomb Crystal ◽  
Screening Parameter

AbstractIn dusty plasma, the overlapping Debye spheres around dust grains produce an attractive force. Shadowing force is exerted between neighboring particles because of mutual distortion of ion or neutral flux to the particles. A comparative study has been made on the role of these two forces on 2D structure of dusty system. Radial distribution function for the particles is a comparative study between the effect of the coupled Yukawa-shadowing potential and the coupled Yukawa-Overlapping Debye Sphere (ODS) potential on 2D dust crystal formation, which has been performed by using molecular dynamics simulation. The structure of the system is investigated by calculating the radial distribution function (g(r)) for different values of Γ, κ and dust number densities nd. It is seen from our study that the Coulomb coupling parameter does not have significant effect on both ODS and shadowing forces. The attractive shadowing force is more dominant for grains with large screening parameter. However, the ODS force becomes dominant with the increasing value of the dust number density. The results for the Yukawa-Shadowing and the ODS potential are also compared with experimental results and a close agreement is obtained for attractive shadowing force.

scholarly journals Inhomogeneous Chiral and Coulomb Crystal in Neutron Stars

2017 ◽  
Vol 13 (S337) ◽  
pp. 428-429
Author(s):  
Nobutoshi Yasutake ◽  
Tong-Gyu Lee ◽  
Toshiki Maruyama ◽  
Toshitaka Tatsumi
Keyword(s):  
Surface Tension ◽  
Simple Model ◽  
Neutron Stars ◽  
Coulomb Interaction ◽  
Condensed Matter ◽  
Chiral Condensate ◽  
Spatial Modulation ◽  
Fflo State ◽  
Coulomb Crystal ◽  
Inhomogeneous Phase

AbstractWe study the possibility of two types of inhomogeneous phases in core of neutron stars: one is the Coulomb crystal, which is known as quark-hadron pasta structures, and another one is chiral crystal. In the Coulomb crystal, the inhomogeneous phase appears as the result of the balance between the surface tension and the Coulomb interaction. In chiral crystal, we study the inhomogeneous chiral condensate, which has spatial modulation. In the simple model in 1+1 dimensions, this condensate has the same feature with the FFLO state, which is well known in the condensed matter physics.

scholarly journals Cooling of White Dwarfs with Account of Non-Equilibrium Beta-Processes

1989 ◽  
Vol 114 ◽  
pp. 269-272
Author(s):  
G.S. Bisnovatyi-Kogan
Keyword(s):  
White Dwarf ◽  
White Dwarfs ◽  
Central Density ◽  
Mass Limit ◽  
Threshold Density ◽  
Finite Density ◽  
Coulomb Crystal ◽  
New Phase ◽  
Non Equilibrium

Non-equilibrium heating of white dwarfs during two-step neutronization and formation of small but finite core of the new phase is a main source of energy in these stars when the temperature is sufficiently small and Coulomb crystal becomes degenerate.Existence of Chandrasekhar mass limit of white dwarfs Mch = 5.83 /μ2z, μz = A/z, is connected with the prevalence of the relativistic degenerate electrons in pressure. When neutronization is taken into account, the maximal value of mass is smaller and is reached at finite density (Schatzman, 1958). The central density of the white dwarf with limiting mass is larger than threshold density of neutronization. Such star has a small, but finite core of new phase (Seidov, 1967). The neutronization threshold for the iron is equal to ρ = 1.15 109 g/cm3 The neutronization goes through two steps

Formation of Coulomb crystal in presence of attractive overlapping Debye sphere potential

2011 ◽  
Vol 18 (9) ◽  
pp. 093702 ◽  
Author(s):  
Swati Baruah ◽  
Nilakshi Das
Keyword(s):  
Coulomb Crystal

Instability of Dust Particles in a Coulomb Crystal due to Delayed Charging

1999 ◽  
Vol 83 (10) ◽  
pp. 1970-1973 ◽  
Author(s):  
S. Nunomura ◽  
T. Misawa ◽  
N. Ohno ◽  
S. Takamura
Keyword(s):  
Dust Particles ◽  
Coulomb Crystal
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