Design and Performance of the New Sartorius 1kg-Prototype Mass Comparator for High Precision Mass Determination and Research Applications

MAN Diesel & Turbo has developed a new gas turbine in the 6 MW-class for both mechanical drive and power generation applications. The lay-out of the Gas Turbine has been driven by opportunities in current and future markets and the positioning of the competition, and this has determined the characteristics and technical parameters which have been optimized in the 6 MW design. The design makes use of extremely high precision engineering so that the assembly of sub components to modules is a smooth flowing process and can guarantee both the high standards in quality and performance which MAN Diesel & Turbo is aiming for. Individual components have been tested and thoroughly validated. These tests include in particular the compressor of the gas turbine and the combustion chamber. The commissioning of the gas turbine prototype engine had been prepared with a numerous number of measuring probes and carried out at the Oberhausen plant gas turbine test field. Results of component and the gas turbine prototype tests will be presented and discussed.

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Astrometry and Spectroscopy as Tools Toward Visual-Binary Masses

International Astronomical Union Colloquium ◽

10.1017/s0252921100006552 ◽

1992 ◽

Vol 135 ◽

pp. 273-275

Author(s):

W.D. Heintz

Keyword(s):

High Precision ◽

Main Sequence ◽

Mass Determination ◽

Orbital Elements ◽

High Quality ◽

Visual Binary ◽

Mass Ratios ◽

The Status ◽

Sequence Components

Following the diversified topic of this conference, let me present a variety of comments — not all new, but resulting from a long string of stars drifting across the desk. The chase after visual orbital elements is not exactly a self-purpose but is aiming at further data, in particular, at good masses. The last published lists of high-quality mass determination represent the status of 20 years ago; but a compilation at this time would probably not last long as the progress promises to quicken.We have 1000 positional (visual/photographic/speckle) orbits, among them about 700 acceptable in the range from fair to definitive. Yet less than 10% of them give good component masses. Most of them are outside the range of parallax measures with the requisite, high precision (that unfortunatly holds for the Hyades); some frustrate the parallax measurer by displaying wedge– and peanut–shaped images, and the more exciting cases of abnormal, non-main–sequence components often cannot get good mass ratios owing to large distances or long periods.

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Asteroseismic Results from WIRE

International Astronomical Union Colloquium ◽

10.1017/s0252921100017267 ◽

2002 ◽

Vol 185 ◽

pp. 616-619 ◽

Cited By ~ 1

Author(s):

D. Buzasi

Keyword(s):

High Precision ◽

And Performance

AbstractThe failed NASA infrared mission WIRE was successfully converted into a high-precision photometry experiment which operated for 17 months. Below I summarize the mission characteristics and performance, as well as providing some examples of the data obtained.

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Design And Performance Of A Dynamically-Programmable High-Precision Threshold Gate

10.1117/12.939920 ◽

1987 ◽

Author(s):

R. Arrathoon ◽

M. H. Hassoun

Keyword(s):

High Precision ◽

And Performance ◽

Threshold Gate

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The Asteroid Mass Determination Project at The U.S. Naval Observatory

International Astronomical Union Colloquium ◽

10.1017/s0252921100072729 ◽

1999 ◽

Vol 172 ◽

pp. 361-362

Author(s):

James L. Hilton ◽

Ronald C. Stone

Keyword(s):

High Precision ◽

Mass Determination ◽

Mean Motion ◽

Naval Observatory ◽

Before And After ◽

Change In The Mean ◽

The Mean ◽

The Masses ◽

The U.S ◽

Better Than

Asteroid masses are the largest source of unmodeled forces in current planetary ephemerides research. Williams (1984) showed that the asteroids produce km size perturbations in the position of Mars. However, the masses of only three asteroids are known to better than 10%, and only six other asteroid masses have been determined at all.Detecting the mass of an asteroid is difficult because the observed quantity is the change in the mean motion of a second, perturbed asteroid. Asteroid masses are small, so the change in the mean motion is typically on the order of 0."015 yr−1. Thus, excellent orbit determinations are needed both before and after the perturbing encounter. This requires high precision observations over as many oppositions as possible.Hilton (1997) determined the mass of 15 Eunomia to within 25% by detecting perturbations of 1313 Berna. The greatest source of uncertainty in determining the mass of Eunomia was the very poor coverage and accuracy of pre-encounter observations. Hilton (1998) has determined the masses of 1 Ceres, 2 Pallas and 4 Vesta, all based on mutual interactions. The uncertainties in the masses are 1% for Ceres, 3% for Pallas, and 7% for Vesta. The masses of Ceres and Pallas are the best so far, and the mass for Vesta corroborates previous determinations of its mass.

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Accurate Binary Mass Determinations: Goals, Limitations, and Prospects

Symposium - International Astronomical Union ◽

10.1017/s0074180900228052 ◽

1995 ◽

Vol 166 ◽

pp. 187-192

Author(s):

J. Andersen

Keyword(s):

High Precision ◽

Binary Stars ◽

State Of The Art ◽

The State ◽

Accurate Mass ◽

Mass Determination ◽

Auxiliary Data ◽

Typical System ◽

Stellar Masses ◽

Precision Astrometry

The state of the art in accurate mass determination for binary stars is reviewed, and the angular sizes and their errors are computed for a typical system from the existing high-precision sample. It appears that sub-μas (microarcsecond) absolute astrometry will be needed in order to improve the accuracy substantially by astrometry alone. The types of system, and the kinds of data, where precision astrometry appears most promising are outlined. Finally, astrophysical applications of such accurate stellar masses, and the auxiliary data required in them, are briefly reviewed.

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