標題: Titlebook: Astrophysical Radiation Hydrodynamics; Karl-Heiz A. Winkler,Michael L. Norman Book 1986 D. Reidel Publishing Company, Dordrecht, Holland 1 [打印本頁] 作者: graphic 時間: 2025-3-21 16:38
書目名稱Astrophysical Radiation Hydrodynamics影響因子(影響力)
作者: BATE 時間: 2025-3-21 20:52 作者: 難理解 時間: 2025-3-22 01:11
WH80s: Numerical Radiation Hydrodynamicsve transfer and its moments are formulated in a fully adaptive coordinate system in space, angle and frequency. Integral conservation laws for the radiation quantities, which form the basis for our method, are then given. A hierarchy of splitting schemes for reducing this 3-dimensional problem to on作者: 復(fù)習(xí) 時間: 2025-3-22 04:53 作者: Astigmatism 時間: 2025-3-22 11:19
Implicit 2D-Radiation Hydrodynamics) and by Bodenheimer and Sweigart (1968), due to the conspicuous non-homology of the gravitational collapse of a (non-rotating, non-magnetic) interstellar cloud on the verge of being Jeans-unstable, both time and length scales vary by several orders of magnitude during the evolution of the cloud. To作者: exclamation 時間: 2025-3-22 15:45
2-D Eulerian Hydrodynamics with Fluid Interfaces, Self-Gravity and Rotationamical problems in astrophysics involving inviscid compressible flow, self-gravitation, rotation, and fluid instabilities of the Rayleigh-Taylor and Kelvin-Helmholtz types. The computer code to be described has been applied most recently to modeling jets in radio galaxies (Norman et al. 1981, 1982) 作者: Ganglion-Cyst 時間: 2025-3-22 19:56 作者: 共棲 時間: 2025-3-22 22:45 作者: embolus 時間: 2025-3-23 04:55
Finite Element Methods for Time Dependent Problemsf methods for solving partial differential equations. Their range of application has expanded inexorably so that they now pervade almost all areas. In certain applications, such as time dependent and fluids problems, finite elements have been in use for only a relatively short period of time and one作者: 展覽 時間: 2025-3-23 08:15
Description and Philosophy of Spectral Methodsferences. For example, the ?. operator in 2 or 3 dimensions is easier to invert with spectral techniques because the spatial dependence of the operator separates in a more natural way. We warn against the use of some of the more common spectral expansions. Bessel series expansions of functions in cy作者: bifurcate 時間: 2025-3-23 11:28 作者: 減少 時間: 2025-3-23 17:35
Particle Methodsarticle methods relate to other approaches (finite difference, finite element and spectral methods) and survey particle methods. Sections 2, 3 and 4 focus respectively on particle-mesh (PM) methods for collisionless systems, particle-particle/particle-mesh (P.m) methods for correlated systems and fl作者: crucial 時間: 2025-3-23 21:16
Why Ultrarelativistic Numerical Hydrodynamics is Difficultn. The numerical code is an adaptation of the WH80s Newtonian radiation hydrodynamics code described by Winkler and Norman in these proceedings. Shock fronts are treated by the method of artificial viscosity. We derive the equations of motion for an ideal gas with artificial viscosity in Eulerian an作者: Isthmus 時間: 2025-3-23 22:23
Neutrino Transport in Relativity black holes. It uses a Lagrangian hydrodynamic formulation as a framework. The method is of mediocre accuracy, but it can handle all cases efficiently. The second method of solving the transport equation is for use in cosmology. In this case all velocities are of the same size and an explicit monot作者: Exaggerate 時間: 2025-3-24 04:26
Numerical Relativistic Gravitational Collapse with Spatial Time Slices while the Lagrangian observer is one at rest in the fluid. We can define an observer at an event in spacetime by giving his 4-velocity at that event. The path through spacetime taken by the observer is called the timeline of that observer. In flat Minkowski spacetime (the spacetime of special relat作者: Microaneurysm 時間: 2025-3-24 08:18 作者: POINT 時間: 2025-3-24 11:58 作者: 高度贊揚 時間: 2025-3-24 17:57
https://doi.org/10.1007/978-1-4302-0158-8. The transport equation for a moving radiating fluid is presented in both a fully Eulerian and a fully Lagrangean formulation, along with conservation equations describing the dynamics of the fluid. Special attention is paid to the problem of deriving equations that are mutually consistent in each 作者: 顯而易見 時間: 2025-3-24 21:12 作者: Minutes 時間: 2025-3-25 00:15 作者: CERE 時間: 2025-3-25 03:35
Foundation ASP for Dreamweaver 8) and by Bodenheimer and Sweigart (1968), due to the conspicuous non-homology of the gravitational collapse of a (non-rotating, non-magnetic) interstellar cloud on the verge of being Jeans-unstable, both time and length scales vary by several orders of magnitude during the evolution of the cloud. To作者: 流眼淚 時間: 2025-3-25 09:34 作者: geometrician 時間: 2025-3-25 15:23 作者: 用手捏 時間: 2025-3-25 16:10 作者: geometrician 時間: 2025-3-25 23:05
Completing the Quotes Administration System,f methods for solving partial differential equations. Their range of application has expanded inexorably so that they now pervade almost all areas. In certain applications, such as time dependent and fluids problems, finite elements have been in use for only a relatively short period of time and one作者: BLUSH 時間: 2025-3-26 04:05 作者: Radiculopathy 時間: 2025-3-26 07:40
Foundation ASP for Dreamweaver 8esolvable, small-scale flow, and show how numerical simulations that neglect the subgrid-scale motions produce erroneous solutions. Then we discuss the “quick fix” remedy of introducing a numerical or eddy-viscosity. We sketch how the analytic theories of turbulence attempt to model the large-scale 作者: 積云 時間: 2025-3-26 12:25
Foundation ASP for Dreamweaver 8article methods relate to other approaches (finite difference, finite element and spectral methods) and survey particle methods. Sections 2, 3 and 4 focus respectively on particle-mesh (PM) methods for collisionless systems, particle-particle/particle-mesh (P.m) methods for correlated systems and fl作者: FLOUR 時間: 2025-3-26 14:32 作者: 拾落穗 時間: 2025-3-26 17:55 作者: 粗糙濫制 時間: 2025-3-27 00:35
https://doi.org/10.1007/978-1-4302-0120-5 while the Lagrangian observer is one at rest in the fluid. We can define an observer at an event in spacetime by giving his 4-velocity at that event. The path through spacetime taken by the observer is called the timeline of that observer. In flat Minkowski spacetime (the spacetime of special relat作者: 鑒賞家 時間: 2025-3-27 04:41 作者: 閑蕩 時間: 2025-3-27 08:55 作者: 使激動 時間: 2025-3-27 11:52 作者: 實施生效 時間: 2025-3-27 17:05 作者: antidote 時間: 2025-3-27 21:18
https://doi.org/10.1007/978-94-009-4754-2astronomy; astrophysics; gravitation; relativity; turbulence作者: 豎琴 時間: 2025-3-28 00:09
978-94-010-8612-7D. Reidel Publishing Company, Dordrecht, Holland 1986作者: RENIN 時間: 2025-3-28 05:25
Nato Science Series C:http://image.papertrans.cn/b/image/163684.jpg作者: micturition 時間: 2025-3-28 07:41
1389-2185 ivistic and relativistic hydrodynamics, radia- tive transfer, and radiation-coupled hydrodynamics. The unifying theme of the lectures was the successful application of these methods to challenging problems in astrophysics. The workshop was subdivided into 3 somewhat independent topics, each with the作者: AMOR 時間: 2025-3-28 11:01 作者: 橡子 時間: 2025-3-28 18:20
Foundation ASP for Dreamweaver 8oyed by observers, is to use image processing techniques. In this method, the original data are carefully screened and processed with enhancement algorithms until the various structures hidden in the image become clearly visible and can be displayed graphically.作者: Credence 時間: 2025-3-28 20:48 作者: insert 時間: 2025-3-28 23:56
Completing the Quotes Administration System, certain applications, such as time dependent and fluids problems, finite elements have been in use for only a relatively short period of time and one can therefore expect further developments to take place to improve their overall efficiency.作者: bile648 時間: 2025-3-29 05:42 作者: Inculcate 時間: 2025-3-29 09:58
Problems in Astrophysical Radiation Hydrodynamicsion in this regime. Further discussion is devoted to two classes of application of these ideas. The first class consists of problems dominated by line radiation, which is sensitive to the velocity field through the Doppler effect. The second class is of problems in which the advection of radiation by moving matter dominates radiation diffusion.作者: Anonymous 時間: 2025-3-29 12:50
Munacolor: Understanding High-Resolution Gas Dynamical Simulations Through Color Graphicsoyed by observers, is to use image processing techniques. In this method, the original data are carefully screened and processed with enhancement algorithms until the various structures hidden in the image become clearly visible and can be displayed graphically.作者: Ophthalmoscope 時間: 2025-3-29 15:37 作者: 切掉 時間: 2025-3-29 23:05
Finite Element Methods for Time Dependent Problems certain applications, such as time dependent and fluids problems, finite elements have been in use for only a relatively short period of time and one can therefore expect further developments to take place to improve their overall efficiency.作者: synovitis 時間: 2025-3-30 02:12
Neutrino Transport in Relativityy. The second method of solving the transport equation is for use in cosmology. In this case all velocities are of the same size and an explicit monotonic second order in space differencing is used. This latter method includes the effects of neutrino rest mass.作者: 百靈鳥 時間: 2025-3-30 04:48
Description and Philosophy of Spectral Methodslindrical geometries converge poorly. However, other series expansions of the same functions converge quickly. We show how to choose basis functions that give fast convergence and outline the differences between Galerkin, tau, modal, collocation, and pseudo-spectral methods.作者: 死亡 時間: 2025-3-30 09:59 作者: addict 時間: 2025-3-30 15:04
The Equations of Radiation Hydrodynamicshe equations, and 2) to solve the equations to 0(v/c) in quite general circumstances..These points will be illustrated in the context of the non-equilibrium radiation diffusion limit, and a sketch of how the Lagrangean equations are to be solved will be presented.作者: 信任 時間: 2025-3-30 17:33 作者: 天賦 時間: 2025-3-30 23:32
Building a Random Quote Generator, symmetry. We also show how to calculate the expected appearance of models for which the source function and extinction coefficient are known. Examples of such calculations are presented and discussed.作者: 冒煙 時間: 2025-3-31 01:01 作者: INCUR 時間: 2025-3-31 07:48
https://doi.org/10.1007/978-1-4302-0120-5rtificial viscous “pressure” in the Eulerian equations of motion. These errors are eliminated in the present code, which gives good results on three test problems involving strong relativistic shock waves.作者: cipher 時間: 2025-3-31 12:00 作者: Expediency 時間: 2025-3-31 16:06
Numerical Modeling of Subgrid-Scale Flow in Turbulence, Rotation, and Convectionhich numerical and eddy-viscosities produce incorrect solutions. Improved models of the subgrid-scale flow are examined. We show how numerical simulation of large Reynolds number (but non-turbulent) flows can guide us in modeling subgrid-scale flows in astrophysical settings.
