AMERICA'S FORESTS: AN ENERGY ENTERPRISE  L. C. Walker is dean and R. R. Hicks, Jr. is associate professor, Stephen F. Austin State University School of Forestry, Nacogdoches, Texas 75961.

Walker, Laurence C.; Hicks, Ray R.

doi:10.1016/b978-0-12-454250-1.50044-7

Cited by 6 publications

(6 citation statements)

References 7 publications

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“…This sample of eclipsing binaries in multiple-star systems represents less than 2% of all known eclipsing binary systems. Undoubtedly the fraction of eclipsing binaries which are members of multiple-star systems is much higher than this, and such a conclusion is implied in the data given by Walker ( 1977). Most of the stars which have been discussed are fairly well observed systems, and nearly all are brighter than 10th magnitude.…”

Section: Discussionmentioning

confidence: 84%

Eclipsing binaries in multiple-star systems

Chambliss

1992

PASP

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About 80 eclipsing binaries are known to be components of multiple-star systems. This is less than 2% of all known eclipsing-binary systems, but the actual total is certainly much higher than this, as the majority of stars under review are in fairly bright, well-studied systems. Triple-star systems are by far the most common of these, but one system in five is a quadruple or higher-order system. Quadruple systems include both systems of hierarchy 2 (two widely spaced pairs, e.g., BV+BW Draconis) and hierarchy 3 (e.g., r] Orionis). V772 Herculis and DN Ursae Majoris are in quintuple systems, and HR 3337 and the system that contains GZ Andromedae may also be quintuple. Castor, which contains the eclipsing binary YY Geminorum, is a very rare example of a sextuple-star system. Also considered are eclipsing binaries in compact star clusters such as SZ Camelopardalis and the two binaries in the Trapezium, BM Ori and V 1016 Ori. The most frequently encountered type of eclipsing binary to be found in multiple-star systems is that composed of two early-type (B5 or earlier) stars. Nearly all of the very close triple systems which have eclipsing-binary components are of this type. W UMa-type stars are also well represented among the multiple-star systems containing eclipsing binaries, but some other types are not. The RS Canum Venaticorum stars occur less frequently as components of multiple-star systems, and cataclysmic binaries appear to occur only very rarely as components of these systems. The physical and orbital properties of the multiple star systems are discussed in some detail in cases where the data are fairly complete, but it must be noted that many of the visual pairs have periods of revolution which are much too long to permit reliable determination of orbits. In triple-star systems with eclipsing binaries the ratio of P 2 /P x ranges from less than 10 (for A Tauri) to more than 10 7 in some cases. The questions of co-planarity of orbits and the membership of components in multiple-star systems are also considered.

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Section: Discussionmentioning

confidence: 84%

Eclipsing binaries in multiple-star systems

Chambliss

1992

PASP

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“…The deposit hardness is generally influenced by three factors: fineness of the grains, the dislocation density and dislocations by impurities. 23,29 The deposits with the smallest grain size have high hardness values. 23 The increase in microhardness of Ni-Co-P deposits annealed to 400uC for 1 h is due to the formation of hardened Ni 3 P phase, as observed by XRD and the formation of fine particles, as observed by SEM.…”

Section: Effect Of Co Content On Microhardness Of Depositsmentioning

confidence: 99%

Electroless deposition of Nickel–cobalt–phosphorus nanoalloy

Srinivasan

Selvaganapathy

Meenakshi³

et al. 2011

Surface Engineering

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Electroless plating have unique metallurgical characteristics, and the deposits can be made onto a wide range of substrates, including both metallic and non-metallic surfaces. In this paper, the authors have reported on the development of new bath formulation for getting Ni-Co-P nanoalloy deposit and optimised bath concentration and operating conditions. The alloy deposit contains 10?59%Co in the Ni-P matrix. There is an increase in hardness and corrosion resistance of the deposit with the incorporation of Co. Furthermore, from the XRD measurements of the deposits, it was found that the alloy is nanocrystalline in nature, and the particle size is around 37-45 nm. Atomic force microscopy results show that the height of the particles is in nanosize, and roughness of the surface is within 3 nm.

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“…Von einem vollstandigen oder gar quantitativen Verstandnis der Reaktion sind wir heute noch weit entfcrnt. Allerdings existieren einige quantitative Modelle [6,7], mit denen man das Verhalten einer makroskopischen Stoffmenge [8] beschreiben kann, ohne die beteiligten Elementarprozesse zu kennen. Derartige formale Reaktionsansatze sind von groi3em praktischem Wert, geben uns aber fur das angestrebte mikroskopische Verstandnis bestenfalls Hinweise auf die kinetisch relevanten Teilschritte.…”

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Zum Mechanismus der Oxidation von elementarem Kohlenstoff mit Sauerstoff

Schlögl

1994

Chemie in nserer Zeit

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Ausgehend von einer Arbeitshypothese eines Reaktionsmechanismus der Oxidation von Kohlenstoff (Abbildung 2) wurden verschiedenartige Experimente vorgestellt, die jeweils einen Teilaspekt dieses Mechanismus belegen sollen. Die Aktivierung von Sauerstoff ist ein mehrstufiger Prozeß über unterschiedliche Zwischenverbindungen. Zunächst läßt sich schwach gebundener molekularer Sauerstoff in chemisorbiertem Zustand nachweisen (Desorptionstemperatur etwa 100 K). Dieser ist Vorläufer für einen stärker gebundenen molekularen Zustand, dessen Bildung eine Aktivierungsenergie etwa der Größe der Desorptionsenergie des Vorläuferzustandes erfordert (Desorptionstemperatur 300 – 400 K). Schließlich konnte eine fest gebundene, atomare Sauerstoffspezies identifiziert werden, deren Angriff auf reaktive Zentren des Substrates wiederum mit einer thermischen aktivierungsenergie der Größe der Desorptionsenergie (Desorptionstemperatur 630 K) zu chemischen Strukturen dieser drei Arten von chemisorbiertem Sauerstoff ist jedoch noch nicht eindeutig gesichert.

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AMERICA'S FORESTS: AN ENERGY ENTERPRISE L. C. Walker is dean and R. R. Hicks, Jr. is associate professor, Stephen F. Austin State University School of Forestry, Nacogdoches, Texas 75961.

Cited by 6 publications

References 7 publications

Eclipsing binaries in multiple-star systems

Eclipsing binaries in multiple-star systems

Electroless deposition of Nickel–cobalt–phosphorus nanoalloy

Zum Mechanismus der Oxidation von elementarem Kohlenstoff mit Sauerstoff

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