High Angular Resolution Measurements of Stellar Properties

McAlister, Harold A.

doi:10.1146/annurev.aa.23.090185.000423

Cited by 35 publications

(6 citation statements)

References 92 publications

(109 reference statements)

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“…Visual and spectroscopic observations yield reliable mass estimates and form the bedrock of stellar evolution theory (e.g., Eggen, 1967). The advent of speckle interferometry and optical long-baseline interferometry has led to a remarkable increase in the data quality and volume of binaries, including many shortperiod binaries for the first time (e.g., McAlister, 1985;Hartkopf et al, 2001). This work allows unprecedented tests of stellar evolution models on a case-by-case basis, through sub-1% precision of stellar parameters.…”

Section: Binary Stars and Stellar Evolutionmentioning

confidence: 99%

Optical interferometry in astronomy

2003

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Abstract. Here I review the current state of the field of optical stellar interferometry, concentrating on ground-based work although a brief report of space interferometry missions is included. We pause both to reflect on decades of immense progress in the field as well as to prepare for a new generation of large interferometers just now being commissioned (most notably, the CHARA, Keck and VLT Interferometers). First, this review summarizes the basic principles behind stellar interferometry needed by the lay-physicist and general astronomer to understand the scientific potential as well as technical challenges of interferometry. Next, the basic design principles of practical interferometers are discussed, using the experience of past and existing facilities to illustrate important points. Here there is significant discussion of current trends in the field, including the new facilities under construction and advanced technologies being debuted. This decade has seen the influence of stellar interferometry extend beyond classical regimes of stellar diameters and binary orbits to new areas such as mapping the accretion disks around young stars, novel calibration of the Cepheid Period-Luminosity relation, and imaging of stellar surfaces. The third section is devoted to the major scientific results from interferometry, grouped into natural categories reflecting these current developments. Lastly, I consider the future of interferometry, highlighting the kinds of new science promised by the interferometers coming on-line in the next few years. I also discuss the longer-term future of optical interferometry, including the prospects for space interferometry and the possibilities of large-scale ground-based projects. Critical technological developments are still needed to make these projects attractive and affordable. †

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Section: Binary Stars and Stellar Evolutionmentioning

confidence: 99%

Optical interferometry in astronomy

2003

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“…This technique not only allowed observations of binaries (stars gravitationally bound to each other) with angular separations below the seeing limit, but the observations were generally an order of magnitude more accurate than visual observations (McAlister 1985). This technique not only allowed observations of binaries (stars gravitationally bound to each other) with angular separations below the seeing limit, but the observations were generally an order of magnitude more accurate than visual observations (McAlister 1985).…”

Section: Speckle Interferometrymentioning

confidence: 99%

Binary star astrometry with milli and sub-milli arcsecond precision

2014

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The past several decades have seen accelerating progress in improving binary stars fundamental parameters determinations, as new observational techniques have produced visual orbits of many spectroscopic binaries with a milli arcsecond precision. Modern astrometry is rapidly approaching the goal of sub-milli arcsecond precision, and although presently this precision has been achieved only for a limited number of binary stars, in the near future this will become a standard for very large number of objects. In this paper we review the representative results of techniques which have already allowed the sub-milli arcsecond precision like the optical long baseline interferometry, as well as the precursor techniques such as speckle interferometry, adaptive optics and aperture masking. These techniques provide a step forward from milli to sub-milli arcsecond precision, allowing even short period binaries to be resolved, and often resulting in orbits allowing precisions in stellar dynamical masses better than 1%. We point out that such unprecedented precisions should allow for a significant improvement of our comprehension of stellar physics and other related astrophysical topics.

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“…The choice of parameters was driven by our interest in stellar studies and by our experience with the Narrabri Stellar Intensity Interferometer (Hanbury Brown et al 1974). The range of stellar studies possible with a long baseline optical interferometer has been reviewed by Davis (1979;1992) and McAlister (1979;1985). The choice of parameters was also based on the recognition that, although a two aperture instrument cannot be used to form images, it can contribute a great deal to studies in stellar astrophysics.…”

Section: Susps Parametersmentioning

confidence: 99%

The Sydney University Stellar Interferometer (SUSI)

Davis

1994

Symp. - Int. Astron. Union

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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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High Angular Resolution Measurements of Stellar Properties

Cited by 35 publications

References 92 publications

Optical interferometry in astronomy

Optical interferometry in astronomy

Binary star astrometry with milli and sub-milli arcsecond precision

The Sydney University Stellar Interferometer (SUSI)

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