The Intensity Interferometer

1975 ◽  
Vol 22 (6) ◽  
pp. 561-561
Author(s):  
W.T. Welford
Keyword(s):  
Intensity Interferometer

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.

scholarly journals Cool star empirical temperature scales

1997 ◽  
Vol 189 ◽  
pp. 127-136
Author(s):  
Michael S. Bessell
Keyword(s):  
The Sun ◽  
Temperature Calibration ◽  
Flux Method ◽  
Cool Star ◽  
Temperature Scales ◽  
Historical Paper ◽  
Cool Stars ◽  
Infra Red ◽  
Michelson Interferometry ◽  
Intensity Interferometer

The empirical temperatures scale for cool stars is generally well established. Temperatures are now known with reasonable precision for stars covering the range of spectral types from A to M. In the historical paper by Code, Davis, Bless and Hanbury Brown (Code et al. 1976), six stars between 10000K and 6500K had radii measured by the intensity interferometer and these six, together with the sun formed the basis of the empirical temperature calibration at the time. Since then, many temperatures have been derived for A-K stars (Blackwell & Lynas-Gray 1994; Alonso et al. 1996a) using the Infra-Red Flux Method (see Megessier 1994,5 and this volume), while lunar occultations (Ridgway et al. 1980) and more recently Michelson interferometry (Di Benedetto & Rabbia 1987; Dyck et al. 1996), have been used to measure the radii of K and M giants. It is a tribute to Hanbury Brown's Intensity Interferometer that temperature scales based on its measurements are essentially unchanged by the new data.

scholarly journals Australian East?West Baseline Interferometer Observations at 2·3 GHz

1972 ◽  
Vol 25 (4) ◽  
pp. 461
Author(s):  
JS Gubbay ◽  
AJ Legg ◽  
DS Robertson
Keyword(s):  
Radio Source ◽  
Operating Frequency ◽  
Deep Space ◽  
Deep Space Network ◽  
Space Network ◽  
East West ◽  
Intensity Interferometer

In 1967 the two Australian stations of the NASA?JPL Deep Space Network, DSS41 at Island Lagoon near Woomera and DSS42 at Tidbinbilla near Canberra, were operated as an intensity interferometer (Gubbay and Robertson 1967). At the operating frequency of 2�3 GHz, the baseline is 9 � 106 wavelengths in extent and runs 15� south of east from DSS41. In the work reported by Gubbay and Robertson, the flux from the radio source 3C 273 was found to be partially correlated. This note concerns later measurement over the same baseline using an intermediate interferometer (Clark 1968).

Interferometry of the intensity fluctuations in light IV. A test of an intensity interferometer on Sirius A

1958 ◽  
Vol 248 (1253) ◽  
pp. 222-237 ◽  
Keyword(s):  
Considerable Extent ◽  
Present Series ◽  
Angular Diameter ◽  
Baseline Length ◽  
Intensity Fluctuations ◽  
Good Agreement ◽  
Made In ◽  
Intensity Interferometer

An experimental intensity interferometer has been constructed with two searchlight mirrors and tested on Sirius. The correlation observed with the two mirrors close together was found to be in good agreement with that expected theoretically. This result supports the prediction, made in part III of the present series, that the performance of an intensity interferometer should not be significantly affected by atmospheric scintillation. Observations of Sirius were carried out with four different baselines and the decrease of correlation with increasing baseline length was found to be consistent with theory. The observed results have been used to derive an experimental value for the angular diameter of Sirius which is in good agreement with the value given by astrophysical theory. The results of this preliminary experiment confirm, to a considerable extent, the general conclusions reached in part III.

Determination of the Space-Time Extension of Centrally Produced Hadronic Matter Using the Intensity Interferometer Technique inppInteractions at 28.5 GeV/c

1977 ◽  
Vol 38 (16) ◽  
pp. 873-876 ◽  
Author(s):  
C. Ezell ◽  
L. J. Gutay ◽  
A. T. Laasanen ◽  
F. T. Dao ◽  
P. Schübelin ◽  
...  
Keyword(s):  
Space Time ◽  
Hadronic Matter ◽  
Time Extension ◽  
Intensity Interferometer

scholarly journals A Study of  2 Velorum with a Stellar Intensity Interferometer

1970 ◽  
Vol 148 (1) ◽  
pp. 103-117 ◽  
Author(s):  
R. Hanbury Brown ◽  
J. Davis ◽  
D. Herbison-Evans ◽  
L. R. Allen
Keyword(s):  
Intensity Interferometer
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