Stellar interferometer tracking experiment (SITE): a precursor mission for multiple-aperture interferometry in space

1994 ◽  
Author(s):  
Samuel L. Crawford ◽  
David W. Miller ◽  
Michael Shao
Keyword(s):  
Stellar Interferometer

scholarly journals SUSI’s Potential for Double Star Research

1992 ◽  
Vol 135 ◽  
pp. 521-526
Author(s):  
John Davis
Keyword(s):  
Angular Resolution ◽  
Double Star ◽  
Double Stars ◽  
Stellar Interferometer ◽  
New Instrument

AbstractThe Sydney University Stellar Interferometer (SUSI) is currently undergoing commissioning and will soon commence its astronomical program in which observations of double stars will form a major component. With its 640-m long North–South array of input siderostats, the new instrument will have unprecedented angular resolution.

Importance of telescope alignment for the performance of a stellar interferometer

1998 ◽  
Author(s):  
Irene L. Porro ◽  
Wesley A. Traub ◽  
Nathaniel P. Carleton
Keyword(s):  
Stellar Interferometer

Influence of the antenna diagram on a stellar interferometer that is suffering from telescope-pointing errors

2002 ◽  
Vol 41 (28) ◽  
pp. 5835 ◽  
Author(s):  
Emmanuel Longueteau ◽  
Laurent Delage ◽  
François Reynaud
Keyword(s):  
Pointing Errors ◽  
Stellar Interferometer

Analysis of the optical layout of the OZIRIS stellar interferometer

2006 ◽  
Vol 73 (4) ◽  
pp. 294 ◽  
Author(s):  
A. V. Bagrov ◽  
G. I. Lebedeva ◽  
V. B. Lakhtikov ◽  
A. A. Rumyantsev ◽  
A. G. Seregin ◽  
...  
Keyword(s):  
Stellar Interferometer ◽  
Optical Layout

Inner Radii of Dust Shells and Stellar Diameters Obtained by an Infrared Stellar Interferometer at 11 Micron Wavelength

1995 ◽  
pp. 447-448
Author(s):  
W. C. Danchi ◽  
M. Bester ◽  
L. J. Greenhill ◽  
C. G. Degiacomi ◽  
N. Geis ◽  
...  
Keyword(s):  
Dust Shells ◽  
Stellar Interferometer ◽  
Stellar Diameters

Angular Diameters and Effective Temperatures of Some Bright Stars

1967 ◽  
Vol 1 (1) ◽  
pp. 7-8
Author(s):  
R. Hanbury Brown
Keyword(s):  
Michelson Interferometer ◽  
Angular Diameter ◽  
Frequency Range ◽  
Fringe Visibility ◽  
Stellar Interferometer ◽  
Effective Temperatures ◽  
Angular Diameters

The Stellar Interferometer at Narrabri Observatory consists of two large reflectors which focus the light from a star on to two photoelectric detectors. The output currents from these detectors contain fluctuations which correspond to fluctuations in the starlight itself. The fluctuations from the two detectors are amplified in the frequency range 10-100 Mc/s and their correlation is measured by a linear multiplier. This correlation is measured as a function of the separation between the two detectors. It can be shown theoretically that the correlation at any given baseline is proportional to the square of the fringe visibility which would be observed by a classical Michelson interferometer. It is therefore possible from observations of the correlation at different baselines to find the angular diameter of a star.

scholarly journals Long Baseline Interferometry and Binary Stars

1983 ◽  
Vol 62 ◽  
pp. 191-201
Author(s):  
John Davis
Keyword(s):  
Binary Stars ◽  
Binary Systems ◽  
Current Status ◽  
Fundamental Properties ◽  
Long Baseline ◽  
Stellar Interferometer ◽  
Spectroscopic Binary ◽  
Future Plans ◽  
Intensity Interferometer

AbstractThe observations of α Vir with the Narrabri Stellar Intensity Interferometer demonstrated the potential of long baseline interferometry for the determination of fundamental properties of double-lined spectroscopic binary systems. Since the completion of the programme with the Narrabri instrument the Chatterton Astronomy Department has been conducting a study aimed at developing a stellar interferometer with limiting magnitude V ≳ +8 and maximum baseline ≳ 1 km (resolution at 500 nm ≲ 7 × 10−5 seconds of arc). The way in which a long baseline interferometer may be used in the study of binary stars is outlined, the requirements for this work are discussed, and the current status and future plans of the Chatterton Astronomy Department’s programme to develop a new long baseline interferometer are summarised.

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