Speckle Observations of Binary Stars with the WIYN Telescope. IV. Differential Photometry

2004 ◽  
Vol 127 (3) ◽  
pp. 1727-1735 ◽  
Author(s):  
Elliott P. Horch ◽  
Reed D. Meyer ◽  
William F. van Altena
Keyword(s):  
Binary Stars ◽  
Differential Photometry

scholarly journals CCD Speckle Observations of Binary Stars from the Southern Hemisphere. III. Differential Photometry

2001 ◽  
Vol 121 (3) ◽  
pp. 1583-1596 ◽  
Author(s):  
Elliott Horch ◽  
Zoran Ninkov ◽  
Otto G. Franz
Keyword(s):  
Southern Hemisphere ◽  
Binary Stars ◽  
Differential Photometry

EMCCD Speckle Measurements, Differential Photometry and Dynamical Masses of Visual Binary Stars

2011 ◽  
Author(s):  
V. S. Tamazian ◽  
J. A. Docobo ◽  
Yu. Yu. Balega ◽  
N. D. Melikian ◽  
E. A. Malogolovets ◽  
...  
Keyword(s):  
Binary Stars ◽  
Visual Binary ◽  
Differential Photometry ◽  
Visual Binary Stars ◽  
Dynamical Masses

scholarly journals Differential Photometry of Binary Stars

1992 ◽  
Vol 135 ◽  
pp. 308-310
Author(s):  
J.S.B. Dick ◽  
M.N. Devaney ◽  
D.H.P. Jones ◽  
R.W. ARGYLE
Keyword(s):  
Binary Stars ◽  
Short Exposure ◽  
One Dimensional ◽  
Differential Photometry

AbstractUsing a short exposure, one dimensional area scanner, a programme of photometry on binary stars with separations <10″ has been initiated; using speckle techniques, photometry of binaries with separations <1″ is possible. We describe the equipment and techniques and present results acquired during commissioning.

RSCVn Stars in the Southern Hemisphere

1979 ◽  
Vol 46 ◽  
pp. 371-384 ◽  
Author(s):  
J.B. Hearnshaw
Keyword(s):  
Light Curve ◽  
Southern Hemisphere ◽  
Orbital Period ◽  
Binary Stars ◽  
Small Amplitude ◽  
Light Variation ◽  
Orbital Phase

RSCVn stars are fully detached binary stars which show intrinsic small amplitude (up to 0.3 amplitude peak-to-peak) light variations, as well as, in most of the known cases, eclipses. The spectra are F to G, IV to V for the hotter component and usually KOIV for the cooler. They are also characterised by abnormally strong H and K emission from the cooler star, or, occasionally, from both components. The orbital and light curve periods are in the range 1 day to 2 weeks. An interesting feature is the migration of the light variations to earlier orbital phase, as the light variation period is shorter than the orbital period by a few parts in 10+4to a few parts in 10+3.

Mass Ratios in Wide Binary Stars

1997 ◽  
Vol 485 (2) ◽  
pp. 785-788 ◽  
Author(s):  
Mauri J. Valtonen
Keyword(s):  
Binary Stars ◽  
Wide Binary ◽  
Mass Ratios

The study of short orbital period of delta scuti pulsating variable stars

2019 ◽  
Vol 15 (S356) ◽  
pp. 407-407
Author(s):  
Abduselam Mohammed
Keyword(s):  
Time Delay ◽  
Orbital Period ◽  
Binary Stars ◽  
Arrival Time ◽  
Periodic Variation ◽  
Variable Stars ◽  
Orbital Elements ◽  
Pulsating Stars ◽  
Delta Scuti ◽  
Arrival Time Delay

AbstractAs a pulsating star moves in its binary orbit, the path length of the light between us and the star varies, leading to the periodic variation in the arrival time of the signal from the star to us (earth). With the consideration of pulsators light arrival time delay effects several new methods which allows using Kepler photometric data (light curves) alone to find binary stars have been recently developed. Among these modern techniques we used binarogram method and we identified that several δSct pulsating stars have companions. The application of these method on detecting long periods(i.e. longer than about 50 d) δSct pulsating stars is not new, but the uniqueness of this study is we verified that it is also applicable to detect and determine the orbital elements of short periods (i.e short orbital period) δSct pulsating stars. With this investigation, we identified the possible way to overcome effects of fictious peaks, even, on the maximum peaks helpful to verify weather the star has companion or not depend up on the existence of the time-delay. Then, we applied the technique on known binary stars and their orbital elements are previously published. Finally, we identified some new short orbital period δSct pulsating stars and obtained their orbital frequency and period with the same procedures. Because of with our attempts we succeeded and verified the applicability of the method (the Binarogram method) on these stars (i.e short orbital period) for the first time, we expect that our present study will play a great role for similar study and to improve our binary statistics.

scholarly journals Physical Parameters and Chemical Composition of Components of the Am-Type Binary System RR Lyncis

1993 ◽  
Vol 138 ◽  
pp. 192-196
Author(s):  
L.S. Lyubimkov ◽  
T.M. Rachkovskaya
Keyword(s):  
Chemical Composition ◽  
Binary System ◽  
Binary Stars ◽  
Spectroscopic Binaries ◽  
Theoretical Modelling ◽  
Physical Parameters ◽  
Accurate Data ◽  
Element Abundances ◽  
Widespread Phenomenon ◽  
Chemical Anomalies

Duplicity is a very widespread phenomenon among Am-stars. For instance, Abt (1961) investigating 25 such stars found out that 22 of them are spectroscopic binaries. However this important phenomenon is ignored usually in chemical composition investigations of Am-stars. Consequently some “mean” element abundances are determined, which can noticeably differ from real abundances in atmospheres of components. Moreover false chemical anomalies can appear, as shown by the theoretical modelling of spectra of binary stars (Lyubimkov, 1989, 1992). Meanwhile accurate data on chemical composition of Am-stars must be considered as observational test for any hypothesis suggested for explanation of these objects.

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