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Livres sur le sujet « Rotational loss »

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Auteur : Grafiati

Publié le 14 mars 2023

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1

Balona, Luis A., Huib F. Henrichs et Jean Michel Le Contel, dir. Pulsation, Rotation and Mass Loss in Early-Type Stars. Dordrecht : Springer Netherlands, 1994. http://dx.doi.org/10.1007/978-94-011-1030-3.

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2

Symposium, International Astronomical Union. Pulsation, rotation, and mass loss in early-type stars : Proceedings of the 162nd symposium of the International Astronomical Union held in Antibes, Juan-les-Pins, France, October 5-8, 1993. Dordrecht : Kluwer Academic, 1994.

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3

Paul, Dunbavin, dir. Atlantis of the west : The case for Britain's drowned megalithic civilization. New York : Carroll & Graf, 2003.

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4

Dunbavin, Paul. Atlantis of the West : The case for Britain's drowned Megalithic civilization. London : Robinson, 2003.

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5

A, Balona Luis, Henrichs Huib F et Medupe Rodney, dir. International Conference on Magnetic Fields in O, B and A Stars : Origin and connection to pulsation, rotation and mass loss : proceedings of a conference held at University of North-West, Mmabatho, South Africa, 27 November - 1 December, 2002. San Francisco, California : Astronomical Society of the Pacific, 2003.

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6

Nguyen, Kim-Phuong, et Chris D. Glover. Anesthetic Considerations for Scoliosis Repair. Sous la direction de Erin S. Williams, Olutoyin A. Olutoye, Catherine P. Seipel et Titilopemi A. O. Aina. Oxford University Press, 2018. http://dx.doi.org/10.1093/med/9780190678333.003.0032.

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Scoliosis is an anatomical deformity caused by a lateral and rotational shift in the thoracolumbar spine. Surgical correction involves wide exposure of the spine for placement of stabilizing rods and can result in significant complications from excessive blood loss and neurologic impairments. These procedures require vigilance to acid-base status, hemodynamic fluctuations, coagulation, temperature maintenance, and neurologic monitoring from anesthesiologists. Other major anesthetic considerations discussed include maintaining the integrity of perfusion to the spinal cord, positioning concerns, optimal technique for neuromonitoring, and pain control in the perioperative period. This chapter presents a case study of a 14-year-old girl with adolescent idiopathic scoliosis who presents for posterior spinal instrumentation and fusion from T4-L4 with autologous bone graft.

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7

Stern, Dr Michael. Dr. Stern's Rotation Diet : Lose Fast. Lose Forever. Seattle Weight Loss Center, 2020.

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8

(Editor), Luis A. Balona, Huib F. Henrichs (Editor) et Jean Michel Le Contel (Editor), dir. Pulsation, Rotation and Mass Loss in Early-Type Stars (International Astronomical Union Symposia). Springer, 1994.

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9

Naqui, Zaf, et David Warwick. Bone and joint injuries of the wrist and forearm. Oxford University Press, 2018. http://dx.doi.org/10.1093/med/9780198757689.003.0004.

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The forearm is a complex quadrilateral structure linked by the proximal and distal radioulnar joints, ligaments, which include the interosseous membrane and triangular cartilage, and several obliquely orientated muscles. A displaced fracture or ligament rupture within this forearm is likely to involve other structures. Treatment requires anatomic recovery of stable function. The ulnar corner can sustain fractures or ligament ruptures which affect stable, pain-free, congruous forearm rotation. The distal radius may fracture after high- or low-energy trauma; anatomic reduction may not be essential in all; inaccuracy may lead to loss of rotation and ulnocarpal abutment but long-term arthritis is unusual. Children’s fractures are managed with consideration of remodeling potential. The scaphoid is vulnerable to non-union; plaster immobilization, early percutaneous fixation, and later bone-grafting all have roles. Salvage for osteoarthritic non-union may reduce pain but compromises function. Rupture of the carpal ligaments may cause substantial disruption and require complex reconstruction.

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Mashhoon, Bahram. Acceleration Kernel. Oxford University Press, 2017. http://dx.doi.org/10.1093/oso/9780198803805.003.0003.

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The phenomenon of spin-rotation coupling provides the key to the determination of the kernel. Imagine an observer rotating in the positive sense about the direction of propagation of an incident plane monochromatic electromagnetic wave of positive helicity. Using the locality postulate, the field as measured by the rotating observer can be determined. If the observer rotates with the same frequency as the wave, the measured radiation field loses its temporal dependence. By a mere rotation, observers could in principle stay at rest with respect to an incident positive-helicity wave. To avoid this possibility, we assume that a basic radiation field cannot stand completely still with respect to an accelerated observer. This basic principle eventually leads to the determination of the kernel and a nonlocal theory of accelerated systems that is in better agreement with quantum mechanics than the standard theory based on the hypothesis of locality.

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11

Zeitlin, Vladimir. Rotating Shallow-Water Models as Quasilinear Hyperbolic Systems, and Related Numerical Methods. Oxford University Press, 2018. http://dx.doi.org/10.1093/oso/9780198804338.003.0007.

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The chapter contains the mathematical background necessary to understand the properties of RSW models and numerical methods for their simulations. Mathematics of RSW model is presented by using their one-dimensional reductions, which are necessarily’one-and-a-half’ dimensional, due to rotation and include velocity in the second direction. Basic notions of quasi-linear hyperbolic systems are recalled. The notions of weak solutions, wave breaking, and shock formation are introduced and explained on the example of simple-wave equation. Lagrangian description of RSW is used to demonstrate that rotation does not prevent wave-breaking. Hydraulic theory and Rankine–Hugoniot jump conditions are formulated for RSW models. In the two-layer case it is shown that the system loses hyperbolicity in the presence of shear instability. Ideas of construction of well-balanced (i.e. maintaining equilibria) shock-resolving finite-volume numerical methods are explained and these methods are briefly presented, with illustrations on nonlinear evolution of equatorial waves.

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12

Boudreau, Joseph F., et Eric S. Swanson. Simulation. Oxford University Press, 2018. http://dx.doi.org/10.1093/oso/9780198708636.003.0015.

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This chapter is devoted to Monte Carlo simulation of stochastic processes, both fundamental processes and those involving radiation transport through macroscopic material. The computation of fundamental processes builds on the treatment of rotations and Lorentz transformations from the previous chapter and expands it with a discussion of computational techniques for the evaluation of Feynman diagrams. The simulation of radiation transport covers electromagnetic processes such as ionization energy loss, bremsstrahlung, and pair production. A discussion of real-life challenges in the simulation of radiation transport is included, as well as a brief discussion of simulation toolkits that are available for solving industrial-strength problems. The discussion is intended to give an overview of some of the principal computational and numerical techniques enabling these toolkits.

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13

Balona, Luis. Magnetic Fields in O, B and a Stars - Origin and Connection to Pulsation, Rotation and Mass Loss : Proceedings, International Conference, Mmabatho, South ... Society of the Pacific Conference Series). Astronomical Society of the Pacific, 2003.

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14

Balona, Luis A., Huib F. Henrichs et Jean Michel Le Contel. Pulsation, Rotation and Mass Loss in Early-Type Stars : Proceedings of the 162nd Symposium of the International Astronomical Union, Held in Antibes-Juan-Les-Pins, France, October 5-8 1993. Springer, 2012.

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15

Dunbavin, Paul. Atlantis of the West. Independently Published, 2017.

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16

Dunbavin, Paul. Atlantis of the West. Constable and Robinson, 2003.

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17

Schrijver, Karel. Habitability of Planets and Moons. Oxford University Press, 2018. http://dx.doi.org/10.1093/oso/9780198799894.003.0010.

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The author takes us to visit Saturn’s moon Titan, and Venus, Mars, and to the unconfirmed planet GJ581d. Although we find unearthly conditions on these bodies’ surfaces today, things were different in the past. Even now, there are oceans deep below Titan’s frozen ice shell that itself sees liquid methane rains and vast ethane-filled lakes. Venus and Mars both had liquid water long ago, while Venus may even have been comfortably warm and humid before modern complex life developed on Earth. Many potentially habitable exoplanets are likely locked in their rotation to always face their star with the same side, causing incredible differences between their day and night sides. This chapter reviews how oceans and atmospheres are lost by the Sun’s magnetism or protected by that of the planets’, how masses of carbon dioxide can be stored in solid limestone, and how habitable zones shift to and from planets.

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