scholarly journals Issues and observations on applications of the constrained-path Monte Carlo method to many-fermion systems

1999 ◽  
Vol 59 (20) ◽  
pp. 12788-12798 ◽  
Author(s):  
J. Carlson ◽  
J. E. Gubernatis ◽  
G. Ortiz ◽  
Shiwei Zhang
Keyword(s):  
Monte Carlo ◽  
Monte Carlo Method ◽  
Fermion Systems

A Monte Carlo method for calculating strength functions in many-fermion systems

1980 ◽  
Vol 93 (3) ◽  
pp. 227-231 ◽  
Author(s):  
S.D. Bloom ◽  
S.M. Grimes ◽  
R.F. Hausman
Keyword(s):  
Monte Carlo ◽  
Monte Carlo Method ◽  
Fermion Systems ◽  
Strength Functions

scholarly journals Self-learning Monte Carlo method and cumulative update in fermion systems

2017 ◽  
Vol 95 (24) ◽  
Author(s):  
Junwei Liu ◽  
Huitao Shen ◽  
Yang Qi ◽  
Zi Yang Meng ◽  
Liang Fu
Keyword(s):  
Monte Carlo ◽  
Monte Carlo Method ◽  
Fermion Systems ◽  
Self Learning

scholarly journals Self-learning quantum Monte Carlo method in interacting fermion systems

2017 ◽  
Vol 96 (4) ◽  
Author(s):  
Xiao Yan Xu ◽  
Yang Qi ◽  
Junwei Liu ◽  
Liang Fu ◽  
Zi Yang Meng
Keyword(s):  
Monte Carlo ◽  
Monte Carlo Method ◽  
Quantum Monte Carlo ◽  
Fermion Systems ◽  
Quantum Monte Carlo Method ◽  
Self Learning

scholarly journals Exact Monte Carlo Method for Continuum Fermion Systems

2000 ◽  
Vol 85 (17) ◽  
pp. 3547-3551 ◽  
Author(s):  
M. H. Kalos ◽  
Francesco Pederiva
Keyword(s):  
Monte Carlo ◽  
Monte Carlo Method ◽  
Fermion Systems

scholarly journals Pauli Potential and Green-Function Monte-Carlo Method for Many-Fermion Systems

1998 ◽  
Vol 25 (1-3) ◽  
pp. 101-113 ◽  
Author(s):  
B. L. G. Bakker ◽  
M. I. Polikarpov ◽  
A. I. Veselov
Keyword(s):  
Monte Carlo ◽  
Monte Carlo Method ◽  
Green Function ◽  
Pauli Potential ◽  
Fermion Systems

Outbursts of comet Schwassmann-Wachmann 1, and the cloud of interplanetary boulders

1974 ◽  
Vol 22 ◽  
pp. 307 ◽  
Author(s):  
Zdenek Sekanina
Keyword(s):  
Monte Carlo ◽  
Monte Carlo Method ◽  
Interplanetary Space ◽  
Porous Matrix ◽  
Maximum Diameter ◽  
Expansion Velocity ◽  
Solid Constituent ◽  
Meteoric Material ◽  
Periodic Comet

AbstractIt is suggested that the outbursts of Periodic Comet Schwassmann-Wachmann 1 are triggered by impacts of interplanetary boulders on the surface of the comet’s nucleus. The existence of a cloud of such boulders in interplanetary space was predicted by Harwit (1967). We have used the hypothesis to calculate the characteristics of the outbursts – such as their mean rate, optically important dimensions of ejected debris, expansion velocity of the ejecta, maximum diameter of the expanding cloud before it fades out, and the magnitude of the accompanying orbital impulse – and found them reasonably consistent with observations, if the solid constituent of the comet is assumed in the form of a porous matrix of lowstrength meteoric material. A Monte Carlo method was applied to simulate the distributions of impacts, their directions and impact velocities.

Structures and crystallization of vacuum-deposited amorphous Se and Sb films

1990 ◽  
Vol 48 (4) ◽  
pp. 140-141
Author(s):  
Makoto Shiojiri ◽  
Toshiyuki Isshiki ◽  
Tetsuya Fudaba ◽  
Yoshihiro Hirota
Keyword(s):  
Monte Carlo ◽  
Electron Microscope ◽  
Monte Carlo Method ◽  
Computer Program ◽  
Radial Distribution ◽  
Film Formation ◽  
Amorphous State ◽  
Two Dimensional ◽  
Amorphous Films ◽  
Binding Condition

In hexagonal Se crystal each atom is covalently bound to two others to form an endless spiral chain, and in Sb crystal each atom to three others to form an extended puckered sheet. Such chains and sheets may be regarded as one- and two- dimensional molecules, respectively. In this paper we investigate the structures in amorphous state of these elements and the crystallization.HRTEM and ED images of vacuum-deposited amorphous Se and Sb films were taken with a JEM-200CX electron microscope (Cs=1.2 mm). The structure models of amorphous films were constructed on a computer by Monte Carlo method. Generated atoms were subsequently deposited on a space of 2 nm×2 nm as they fulfiled the binding condition, to form a film 5 nm thick (Fig. 1a-1c). An improvement on a previous computer program has been made as to realize the actual film formation. Radial distribution fuction (RDF) curves, ED intensities and HRTEM images for the constructed structure models were calculated, and compared with the observed ones.

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