Last edited by Karamar
Thursday, May 14, 2020 | History

2 edition of High precision optical interferometry and application to Be stars. found in the catalog.

High precision optical interferometry and application to Be stars.

Christopher Tycner

# High precision optical interferometry and application to Be stars.

## by Christopher Tycner

Published .
Written in English

A new technique for calibrating optical long-baseline interferometric observations is developed where both the calibration corrections and the source characteristics are obtained from the observations of a program star. This calibration technique can only be applied to certain classes of objects, such as emission line sources or binary systems, where the parameters describing the characteristics of the source have different functional dependence than the calibration parameters. To demonstrate its effectiveness, the technique is applied to observations of four different Be stars obtained with the Navy Prototype Optical Interferometer. The interferometric observations utilize measurements obtained simultaneously in many spectral channels covering a wide spectral range, where only two channels contain a strong signal due to the circumstellar envelope in the Halpha emission line. The calibrated observations in Halpha allow modeling of the circumstellar envelopes of all four stars with circularly symmetric and elliptical Gaussian models. The best-fit model parameters are then combined with similar results for other Be stars, already published in the literature, to study the relationship between the Ha emission and the physical extent of the Halpha-emitting circumstellar region. For the first time, a clear dependence of the net Halpha emission on the extent of the circumstellar region is demonstrated. These results are consistent with an optically thick line emission that is directly proportional to the effective area of the emitting disk. Within the small sample of stars considered in this analysis, no clear dependence on the spectral type or stellar rotation is established, although the results do suggest that hotter stars might have more extended circumstellar regions.

The Physical Object
Pagination149 leaves.
Number of Pages149
ID Numbers
Open LibraryOL19886877M
ISBN 100612942414

Abstract: We present the first results from an ongoing survey for multiplicity among the bright stars using the Navy Precision Optical Interferometer (NPOI). We first present a summary of NPOI observations of known multiple systems, including the first detection of the companion of $\beta$ Scuti with precise relative astrometry, to illustrate the instrument's detection sensitivity for binaries Cited by: 6. Equipment needed: Pasco precision interferometry kit, a laser, Na lamp, adjustable-hight platform. To simplify the alignment of a Michelson interferometer, it is convenient to work with diverging optical beams. In this case an interference pattern will look like a set of concentric bright and dark circles, since theFile Size: KB.

The extension of multi-telescope interferometry and aperture synthesis to infrared and optical wavelengths will enable in this decade significant progress in stellar and galactic physics, and will lead to great interferometric infrared/optical arrays of the future. The real-time correction of. The design of high frequency antennas: Delannoy, J. Correlators for interferometry - Today and tomorrow: Yoshihiro, Chikada: The use of optical fibres in radioastronomy: Young, Alan C. The multi frequency front end - A new type of front end for the Westerbork Synthesis Radio Telescope: Tan, G. H. Hardware considerations for high.

The application of interferometry to astronomy comes via the van Cittert–Zernike theorem, which states that the correlation of the radiation gathered by two widely spaced telescopes pointing at the same object is proportional to one spatial Fourier component of that object. Once enough Fourier components have been measured, one can perform an inverse transform and produce a by: 1. The RP Photonics Buyer's Guide contains 45 suppliers for optical metrology equipment. Among them: TOPTICA Photonics. TOPTICA offers laser sources for various applications and optical metrology, including time and frequency measurements, tests of fundamental constants and tests of fundamental theories, a term interferometry, laser-based trace gas analysis, and the measurement of smallest.

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### High precision optical interferometry and application to Be stars by Christopher Tycner Download PDF EPUB FB2

Interferometry is a family of techniques in which waves, usually electromagnetic waves, are superimposed, causing the phenomenon of interference, which is used to extract information.

Interferometry is an important investigative technique in the fields of astronomy, fiber optics, engineering metrology, optical metrology, oceanography, seismology, spectroscopy (and its applications to.

When the first edition of Optical Interferometry was published, interferometry was regarded as a rather esoteric method of making measurements, largely confined to the laboratory.

Today, however, besides its use in several fields of research, it has applications in fields as diverse as measurement of length and velocity, sensors for rotation, acceleration, vibration and electrical and magnetic 5/5(1).

In optical astronomy, interferometry is used to combine signals from two or more telescopes to obtain measurements with higher resolution than could be obtained with either telescopes individually. This technique is the basis for astronomical interferometer arrays, which can make measurements of very small astronomical objects if the telescopes are spread out over a wide area.

One of the first uses of optical interferometry was applied by the Michelson stellar interferometer on the Mount Wilson Observatory's reflector telescope to measure the diameters of stars. The red giant star Betelgeuse was the first to have its diameter determined in this way on Decem In the s radio interferometry was used to perform the first high resolution radio astronomy.

Using the optical interferometry techniques it is possible to measure the optical and structural properties of the natural, optical, and synthetic fibers with a high degree of accuracy (Barakat Author: P. Hariharan. "The advantage of interferometry for optical astronomers is that it can provide measurements of stars with a higher angular resolution than is possible with conventional telescopes.

The goals of atomic, molecular, and optical physics (AMO physics) are to elucidate the fundamental laws of physics, to understand the structure of matter and how matter evolves at the atomic and molecular levels, to understand light in all its manifestations, and to create new techniques and devices.

The principle of the optical fiber interferometric measurement system is shown in Fig. employing a broadband light source and a fiber Bragg grating (FBG) as an in-fiber reflective mirror, an optical fiber Michelson interferometer which performs the measurement task and is stabilized with an electronic feedback loop to erase the influences that are resulted from the environmental Author: Sen Ma, Fang Xie, Yunzhi Wang, Liang Chen.

Christopher Tycner has written: 'High precision optical interferometry and application to Be stars' Asked in Astronomy How we know the distance to the pleiades star cluster. Optical interferometry in astronomy is resolved by an interferometer if the fringe contrast goes to zero at the longest baseline.

As motivated in the last paragraph, this occurs when the angular separation is λ/2b, where b is the Size: 2MB. Surveying the Bright Stars by Optical Interferometry I: A Search for Multiplicity Among Stars of Spectral Types F K D.

Hutter, 1R. Zavala, C. Tycner,2 J. Benson,1 C. Hummel,3 J. Sanborn,4 O. High precision mass determinations are potentially possible for SB1. demonstrating that spatial interferometry was feasible. Over the last decade, high angular resolution methods have matured considerably so that spatial interferometry and adaptive optics (see experiment adaptive optics) have become standard observing techniques, and spatial interferometry has gone beyond the measurement of stellar diameters File Size: KB.

A high precision step height measurement system of optical fiber multiplexed interferometry Article in Measurement – January with 30 Reads How we measure 'reads'.

This book, first published inwas the first on optical stellar interferometry. It covers the history, theory and future uses of interferometeric techniques.

It discusses ideas and instruments used in interferometry for advanced students in physics, optics, and Cited by: Surface figure, irregularity, radii, transmitted wavefront error, aberrations, 90 Deg angles, beam deviation (transmitted and reflected), wedge magnitude/parallelism, slope magnitude, and homogeneity testing are just some of the analysis that Precision Optical can perform.

Interferometry applied. In order to generate an interference pattern with high precision (distinct fringes), it is very important to have a single highly stable wavelength source, which is achieved using the XL laser. There are different interferometer set up's based on Michelson's principle, however, the linear set up is the simplest type to explain.

Optical measurement provides a simple, easy, accurate and reliable means for carrying out inspection and measurements in the industry the projected image should be clear, sharp and dimensionally accurate. Application of interference of light is extreme interest in metrologyFile Size: 1MB.

Michelson interferometer is a tool to produce interference between two beams of light. It is the most common design for optical interferometry and was invented by Albert Abraham : Azooptics.

'In this slim and very readable book David F. Buscher does a fantastic job of providing a textbook, that covers the theory of using interferometry at optical and near infrared wavelengths that also provides a wealth of practical advice on all aspects of optical by: 3.

The mixed optical signal is carried by a fiber optic pickup to measurement electronics, where it is converted to a displacement. Summary Interferometry can address a wide variety of metrology applications with high precision and high resolution and without risk of damage to the sample under test.

New applications can be tackled by combining. Under realistic conditions, a precision about μ m was achieved for a distance of m. With a precision that exceeds requirements, the frequency scanned interferometry is a promising high-precision optical alignment technique for International Linear Collider silicon tracker by: Optical interferometer, instrument for making precise measurements for beams of light of such factors as length, surface irregularities, and index of refraction.

It divides a beam of light into a number of beams that travel unequal paths and whose intensities, when reunited, add or subtract.Optical Interferometry and Industrial Interferometers - a Tutorial - Friedemann Mohr Pforzheim University of Applied Sciences Outline 1 Physical Basics and components 2 Interferometry for path measurement 3 Laser vibrometry for vibration measurement The photoelectric conversion process Detecting a light wave Components I: Lenses, beam transformation Components II: Mirrors and retroreflectors.