Effects of impurity on two-dimensional melting transitions

1998 ◽  
Vol 57 (15) ◽  
pp. 9270-9273 ◽  
Author(s):  
Jian Ma ◽  
Eleanor D. Carter ◽  
Hillary B. Kleinberg
2017 ◽  
Vol 7 (2) ◽  
Author(s):  
Joshua A. Anderson ◽  
James Antonaglia ◽  
Jaime A. Millan ◽  
Michael Engel ◽  
Sharon C. Glotzer

2019 ◽  
Vol 10 (11) ◽  
pp. 2924-2930 ◽  
Author(s):  
Nabeel S. Dahod ◽  
Watcharaphol Paritmongkol ◽  
Alexia Stollmann ◽  
Charles Settens ◽  
Shao-Liang Zheng ◽  
...  

1995 ◽  
Vol 99 (41) ◽  
pp. 15269-15278 ◽  
Author(s):  
Michael J. Hostetler ◽  
William L. Manner ◽  
Ralph G. Nuzzo ◽  
Gregory S. Girolami

1966 ◽  
Vol 24 ◽  
pp. 118-119
Author(s):  
Th. Schmidt-Kaler

I should like to give you a very condensed progress report on some spectrophotometric measurements of objective-prism spectra made in collaboration with H. Leicher at Bonn. The procedure used is almost completely automatic. The measurements are made with the help of a semi-automatic fully digitized registering microphotometer constructed by Hög-Hamburg. The reductions are carried out with the aid of a number of interconnected programmes written for the computer IBM 7090, beginning with the output of the photometer in the form of punched cards and ending with the printing-out of the final two-dimensional classifications.


1966 ◽  
Vol 24 ◽  
pp. 3-5
Author(s):  
W. W. Morgan

1. The definition of “normal” stars in spectral classification changes with time; at the time of the publication of theYerkes Spectral Atlasthe term “normal” was applied to stars whose spectra could be fitted smoothly into a two-dimensional array. Thus, at that time, weak-lined spectra (RR Lyrae and HD 140283) would have been considered peculiar. At the present time we would tend to classify such spectra as “normal”—in a more complicated classification scheme which would have a parameter varying with metallic-line intensity within a specific spectral subdivision.


1966 ◽  
Vol 25 ◽  
pp. 46-48 ◽  
Author(s):  
M. Lecar

“Dynamical mixing”, i.e. relaxation of a stellar phase space distribution through interaction with the mean gravitational field, is numerically investigated for a one-dimensional self-gravitating stellar gas. Qualitative results are presented in the form of a motion picture of the flow of phase points (representing homogeneous slabs of stars) in two-dimensional phase space.


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