Development progress of the prototype long baseline optical interferometer in China

The Sydney University Stellar Interferometer has been designed and constructed as a two aperture, single ro, long baseline, optical interferometer with wavefront-tilt compensation and dynamic optical path length compensation. Initially it will operate in the blue part of the visual spectrum but provision has been made for the addition of an additional beam-combining system for a second spectral band. The rationale behind the choice of instrumental parameters, the potential developments which have been taken into account in its construction, and the current status of SUSI are outlined.

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Observations of Nova Cygni 1992 with a long-baseline optical interferometer

The Astronomical Journal ◽

10.1086/116710 ◽

1993 ◽

Vol 106 ◽

pp. 1118 ◽

Cited By ~ 15

Author(s):

A. Quirrenbach ◽

N. M., II Elias ◽

D. Mozurkewich ◽

J. T. Armstrong ◽

D. F. Buscher ◽

...

Keyword(s):

Optical Interferometer ◽

Long Baseline

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Observations of the Triple Star ETA Virginis with a Long Baseline Optical Interferometer

International Astronomical Union Colloquium ◽

10.1017/s0252921100008411 ◽

2004 ◽

Vol 191 ◽

pp. 41-44

Author(s):

C.A. Hummel

Keyword(s):

Spectroscopic Data ◽

Model Fitting ◽

Mass Ratio ◽

Optical Interferometer ◽

Orbital Inclination ◽

Close Pair ◽

Long Baseline ◽

Triple Star ◽

Three Components

AbstractWe observed the hierarchical triple star Eta Virginis with the Navy Prototype Optical Interferometer and present the first images resolving all three components. The stars in the close pair have a separation between 4 and 9 milliarcseconds. The orbital motions of the stars were followed during the winter and spring of 2002. Preliminary, astrometrically determined orbits of the two components in the close pair by reference to the tertiary were derived, thus enabling the estimation of the mass ratio (1.27) of the components in the close pair. We also determined the relative orbital inclination to be 31 degrees. We describe the model-fitting process to interferometrie and spectroscopic data, and discuss some astrophysical component parameters.

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Spatially resolving the wind and disk structures around active B-type stars

Proceedings of the International Astronomical Union ◽

10.1017/s174392131101074x ◽

2010 ◽

Vol 6 (S272) ◽

pp. 337-341

Author(s):

Christopher Tycner

Keyword(s):

Variable Star ◽

Numerical Models ◽

Circumstellar Disk ◽

Physical Parameters ◽

Optical Interferometer ◽

Spatially Resolved ◽

Long Baseline ◽

Early Type Stars ◽

First Time ◽

Luminous Blue Variable

AbstractLong-baseline optical and IR interferometers now routinely resolve the wind and disk-like structures around early-type stars. The typical angular scales resolved by current generation of instruments are well bellow the milli-arcsecond level. These type of observations allow, in some cases for the first time, placing very tight constraints on current theories and models of the circumstellar structures around these type of stars. Specific examples of observations obtained at the Navy Prototype Optical interferometer of the spatially resolved regions around a luminous blue variable star P Cyg and a B-type star with circumstellar disk are presented. The need for connection between interferometric observables and physical parameters predicted by theory and numerical models are emphasized.

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