Duplex system configuration in passive double star system

2002 ◽  
Author(s):  
Y. Okumura ◽  
S. Aoyagi ◽  
E. Maekawa
Keyword(s):  
Double Star ◽  
Star System ◽  
System Configuration ◽  
Duplex System

scholarly journals The Variable Shell Star HR 5999

1977 ◽  
Vol 42 ◽  
pp. 137-143
Author(s):  
P.S. Thé ◽  
H.R.E. Tjin A Djie
Keyword(s):  
Spectral Type ◽  
Proper Motion ◽  
Main Sequence ◽  
Angular Separation ◽  
Double Star ◽  
Star System ◽  
Spectroscopic Observations ◽  
Photometric Observations ◽  
Shell Star ◽  
Hydrogen Lines

From spectroscopic observations Bessell and Eggen (1972) (hereafter called BE) have detected that HR 5999 (erroneously named HR 6000 by BE) is a shell star of spectral type A7 III-IV with hydrogen lines in emission. Photometric observations show subsequently that HR 5999 varies in brightness up to about 1 mag semiregularly with a period of about 1 month. Eggen (1975) believes that HR 5999 forms a pre-main sequence object.With HR 6000, the star HR 5999 forms a visual double star system named Δ199; HR 5999 is the southern component. The angular separation is about 45”. BE show that these stars have a common proper motion, and are, therefore, believed to form a physical pair.

Key technologies for passive double star system

2002 ◽  
Author(s):  
S. Makino ◽  
M. Akita ◽  
Y. Asashiba ◽  
T. Chikazawa ◽  
F. Hidani ◽  
...  
Keyword(s):  
Double Star ◽  
Star System ◽  
Key Technologies

scholarly journals THE ENERGY OF DOUBLE-STAR SYSTEM AND ITS DISTRIBUTION

1979 ◽  
Vol 28 (2) ◽  
pp. 152
Author(s):  
LIU YOU-CHANG
Keyword(s):  
Double Star ◽  
Star System

scholarly journals A photometric search for ‘5-min’ oscillations in the components of Alpha Centauri and two other double stars

1988 ◽  
Vol 123 ◽  
pp. 253-254
Author(s):  
L. A. Balona ◽  
F. Marang
Keyword(s):  
Small Amplitude ◽  
Signal To Noise Ratio ◽  
Broad Band ◽  
Double Star ◽  
The Other ◽  
The Sun ◽  
Star System ◽  
Signal To Noise ◽  
Double Stars ◽  
Wide Range

The discovery of global solar 5-min oscillations has prompted the search for such oscillations in other stars. The main problem in detecting these variations is their expected small amplitude (in the sun it is less than 1 m/s in velocity and 10−6 in integrated light). Two recent studies by Fossat et al. (1984) and Noyes et al. (1984) have suggested that the 5-min oscillations in α Cen and ε Eri may have been detected.We attempted to detect these oscillations by means of conventional broad-band photometry in the components of three double star systems (α Cen, HR4677 and HR5568). We selected these stars because they cover a wide range of spectral types (F2V to M2V). It was hoped that there may be a region where the pulsation amplitudes are particularly large. By using one component of a double star system to correct for transparency variations in the other, we also expected to obtain a larger signal-to-noise ratio.

Multi-bit rate passive double star system using time-unit packet

2001 ◽  
Vol 19 (2) ◽  
pp. 150-158 ◽  
Author(s):  
S. Kobayashi ◽  
Y. Fukada ◽  
M. Hashimoto
Keyword(s):  
Double Star ◽  
Star System ◽  
Bit Rate
Sign in / Sign up

Export Citation Format

Share Document