Weighted two-dimensional longitudinal impedance for driving support system

Author(s):  
J.C.F. de Winter ◽  
M. Mulder ◽  
M.M. van Paassen ◽  
T. Yamamura
2012 ◽  
Vol 27 ◽  
pp. 193-199 ◽  
Author(s):  
Elizabeth Erasmus ◽  
Peter C. Thüne ◽  
M.W.G.M. (Tiny) Verhoeven ◽  
J.W. (Hans) Niemantsverdriet ◽  
Jannie C. Swarts

2013 ◽  
Vol 21 (2) ◽  
pp. 199-210 ◽  
Author(s):  
Tetsuya Miyagawa ◽  
Yoshio Yamagishi ◽  
Shun Mizuno

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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