標題: Titlebook: Computational Methods in Transport; Granlibakken 2004 Frank Graziani Conference proceedings 2006 Springer-Verlag Berlin Heidelberg 2006 App [打印本頁] 作者: Washington 時間: 2025-3-21 18:00
書目名稱Computational Methods in Transport影響因子(影響力)
書目名稱Computational Methods in Transport影響因子(影響力)學科排名
書目名稱Computational Methods in Transport網(wǎng)絡(luò)公開度
書目名稱Computational Methods in Transport網(wǎng)絡(luò)公開度學科排名
書目名稱Computational Methods in Transport被引頻次
書目名稱Computational Methods in Transport被引頻次學科排名
書目名稱Computational Methods in Transport年度引用
書目名稱Computational Methods in Transport年度引用學科排名
書目名稱Computational Methods in Transport讀者反饋
書目名稱Computational Methods in Transport讀者反饋學科排名
作者: MAIZE 時間: 2025-3-21 23:30
https://doi.org/10.1007/978-3-642-57654-6ransport equation is solved by the Symbolic Implicit Monte Carlo (SIMC) method and a comparison is made between the standard formulation and the difference formulation. The SIMC method is easily adapted to the derivative source terms of the difference formulation, and a remarkable reduction in noise作者: JOT 時間: 2025-3-22 02:29 作者: 事與愿違 時間: 2025-3-22 08:14 作者: 喃喃訴苦 時間: 2025-3-22 10:08 作者: 描述 時間: 2025-3-22 14:34 作者: 描述 時間: 2025-3-22 20:46 作者: 俗艷 時間: 2025-3-22 22:58
An Evaluation of the Difference Formulation for Photon Transport in a Two Level Systemmay limit the advantage of the method. We bypass this problem by using the gray approximation. We develop three Monte Carlo solution methods based on different degrees of implicitness for the treatment of the source terms, and we find only conditional stability unless the source terms are treated fully implicitly.作者: In-Situ 時間: 2025-3-23 03:28 作者: Asseverate 時間: 2025-3-23 05:55
Radiative Transfer in Astrophysical Applicationsonomical objects the radiation is so strong that it significantly contributes to the energy and momentum budget of the medium. Therefore, radiation is not only a . of the physical state, but is in fact an .. In other words, radiation in fact . the structure of the medium, yet the medium is probed . by this radiation.作者: 是比賽 時間: 2025-3-23 13:27
Neutrino Transport in Core Collapse Supernovae balance between the electron pressure and gravity is only marginally stable. As a result of electron capture on the free protons and nuclei in the core and as a result of nuclear dissociation under the extreme densities and temperatures, electron and thermal pressure support are reduced, and the core becomes unstable and collapses.作者: 偽書 時間: 2025-3-23 15:05
Effective Propagation Kernels in Structured Media with Broad Spatial Correlations, Illustration withultiple scattering and effective medium theory are examined. Finally, we describe a novel one-dimensional transport theory with asymptotically power-law propagation kernels and use it to shed new light onto recent observations of solar photon pathlength in the Earth’s cloudy atmosphere.作者: fallible 時間: 2025-3-23 19:26
Vegetation Canopy Reflectance Modeling with Turbid Medium Radiative Transferorientation. The presentation concludes with a demonstration of . in a multiple pixel mode to estimate the amount of ripe coffee cherries at harvest in the fields of the Kauai Coffee Company and to detect targets hidden beneath canopies.作者: 昏迷狀態(tài) 時間: 2025-3-23 22:33 作者: Esalate 時間: 2025-3-24 05:45
https://doi.org/10.1007/978-3-319-22759-7collapse supernovae and active galactic nuclei to the formation of stars and planets to cosmological simulations of the first stars. In this paper, we review the current “state-of-the-art” radiation hydrodynamics techniques used in astrophysics.作者: Injunction 時間: 2025-3-24 09:12
Wolfgang Schulz,Toufik Al Khawliswer on a simple question like how significant the 3D effects are for a given problem. The perturbation method is what comes to mind first if we need to go further into modelling of the radiative transfer through cloud atmosphere starting from the simplest framework of one dimensional radiative transfer [2, 8].作者: 同位素 時間: 2025-3-24 11:14
Hydrogen Plasma Reduction of Iron Oxidesy into material energy. Accuracy in time integration is essential for a good solution since a major fraction of the fuel can be depleted in a very short time. Such systems arise in a number of application areas including evolution of a star [1] and inertial confinement fusion [2].作者: Communal 時間: 2025-3-24 16:41 作者: Obstreperous 時間: 2025-3-24 22:19 作者: PATRI 時間: 2025-3-25 00:35 作者: malign 時間: 2025-3-25 04:57
Implicit Solution of Non-Equilibrium Radiation Diffusion Including Reactive Heating Source in Materiy into material energy. Accuracy in time integration is essential for a good solution since a major fraction of the fuel can be depleted in a very short time. Such systems arise in a number of application areas including evolution of a star [1] and inertial confinement fusion [2].作者: 惡意 時間: 2025-3-25 10:47 作者: PANG 時間: 2025-3-25 14:22
Iveta Zolotová,Marek Bundzel,Tomá? Lojka balance between the electron pressure and gravity is only marginally stable. As a result of electron capture on the free protons and nuclei in the core and as a result of nuclear dissociation under the extreme densities and temperatures, electron and thermal pressure support are reduced, and the core becomes unstable and collapses.作者: monogamy 時間: 2025-3-25 17:56 作者: 莊嚴 時間: 2025-3-25 23:54
https://doi.org/10.1007/978-3-319-12304-2orientation. The presentation concludes with a demonstration of . in a multiple pixel mode to estimate the amount of ripe coffee cherries at harvest in the fields of the Kauai Coffee Company and to detect targets hidden beneath canopies.作者: 顯而易見 時間: 2025-3-26 00:40
Marco Hübner,Philipp Jahn,Gregor Tewaagn of non-relativistic material velocities. For simplicity, we next focus on a model of radiative transfer in a static medium that is adequate for the purpose of describing numerical discretization and solution techniques for the transfer equation that can also be applied in the more general context of radiationhydrodynamics.作者: 云狀 時間: 2025-3-26 05:13 作者: Digest 時間: 2025-3-26 10:53
Discrete-Ordinates Methods for Radiative Transfer in the Non-Relativistic Stellar Regimen of non-relativistic material velocities. For simplicity, we next focus on a model of radiative transfer in a static medium that is adequate for the purpose of describing numerical discretization and solution techniques for the transfer equation that can also be applied in the more general context of radiationhydrodynamics.作者: Bravado 時間: 2025-3-26 13:12 作者: 人充滿活力 時間: 2025-3-26 19:39
https://doi.org/10.1007/3-540-28125-8Approximation; Monte Carlo method; algorithms; astrophysics; computational physics; density; diffusion; dyn作者: NEX 時間: 2025-3-27 00:16 作者: Resign 時間: 2025-3-27 04:51 作者: fatuity 時間: 2025-3-27 06:17 作者: Charitable 時間: 2025-3-27 11:47
https://doi.org/10.1007/978-3-319-22759-7ave (and will ever have) about distant objects (exceptions are detected neutrinos from the Sun and supernova SN1987a, and in a near future the gravitational waves). However, there is an even more compelling reason for the a need to deal with detailed radiation transport in astrophysics: In many astr作者: Feedback 時間: 2025-3-27 15:44 作者: 有惡意 時間: 2025-3-27 20:08
Marco Hübner,Philipp Jahn,Gregor Tewaaggime. We consider the non-relativistic regime to be characterized by material velocities less than or equal to one percent of the speed of light. In most applications, the radiative transfer equations are coupled to the hydrodynamics equations. We first describe a radiation-hydrodynamics model that 作者: Exploit 時間: 2025-3-27 23:11
Advances in Production Technologycludes the mean-free-path, one can use an effective propagation kernel that will necessarily be sub-exponential. We come to this conclusion using both standard transport theory for variable media and a point-process approach developed recently by A. Kostinski. The ramifications of this finding for m作者: 敵意 時間: 2025-3-28 02:27 作者: WITH 時間: 2025-3-28 09:43
Wolfgang Schulz,Toufik Al Khawlich as Monte Carlo [12], or SHDOM [3]. However, it is usually required too much time to make a simulation which is inconvenient when just we need an answer on a simple question like how significant the 3D effects are for a given problem. The perturbation method is what comes to mind first if we need 作者: 努力趕上 時間: 2025-3-28 14:24
https://doi.org/10.1007/978-3-319-12304-2f four possible canopy reflectance models. The overview is followed by the description of the . coupled leaf/canopy turbid medium reflectance model based on natural averaging. The model follows conventional radiative transfer theory with modification for canopy architecture as characterized by leaf 作者: Flawless 時間: 2025-3-28 18:38
Advances in Production Technologyes (climate change, environmental degradation, biodiversity preservation, etc.) but also to provide appropriate initial state and boundary conditions for general circulation or landscape succession models. In particular, the 3-D structure of vegetation emerged as a crucial player in processes affect作者: corpus-callosum 時間: 2025-3-28 21:29 作者: anchor 時間: 2025-3-28 23:12
https://doi.org/10.1007/978-3-642-57654-6nd stability of the difference formulation within the framework of the Symbolic Implicit Monte Carlo method. The difference formulation, introduced for thermal radiation by some of the authors, has the unique property that the transport equation is written in terms that become small for thick system作者: Conserve 時間: 2025-3-29 06:59 作者: 格言 時間: 2025-3-29 11:13
Hydrogen Plasma Reduction of Iron Oxidesion with material energy transfer and a fusion fuel source. In certain parameter regimes this system can lead to a rapid conversion of potential energy into material energy. Accuracy in time integration is essential for a good solution since a major fraction of the fuel can be depleted in a very sho作者: START 時間: 2025-3-29 13:14 作者: 誘導 時間: 2025-3-29 18:21 作者: Parabola 時間: 2025-3-29 21:34 作者: osteocytes 時間: 2025-3-30 01:47
Stefan Graichen,Thorsten Stein,Barbara DemlA general introduction to the field of ocean optics is presented, including features that make optical oceanography problems similar to and different from other transport problems. Methods for solving time-independent, one-dimensional problems are discussed that are appropriate for passive illumination conditions.作者: calorie 時間: 2025-3-30 07:49 作者: emulsify 時間: 2025-3-30 08:50 作者: 溫室 時間: 2025-3-30 16:21
Finite-Difference Methods Implemented in SATURN Complex to Solve Multidimensional Time-Dependent TraNumerical simulation of multidimensional particle transport problems falls into the category of the most complex and labor-intensive application problems.作者: 尾巴 時間: 2025-3-30 19:34
Radiation Hydrodynamics in Astrophysics, radiation hydrodynamics codes are being used in a growing number of astrophysics problems from energetic out flows of compact remnants such as core-collapse supernovae and active galactic nuclei to the formation of stars and planets to cosmological simulations of the first stars. In this paper, we作者: 杠桿支點 時間: 2025-3-30 22:38
Radiative Transfer in Astrophysical Applicationsave (and will ever have) about distant objects (exceptions are detected neutrinos from the Sun and supernova SN1987a, and in a near future the gravitational waves). However, there is an even more compelling reason for the a need to deal with detailed radiation transport in astrophysics: In many astr作者: explicit 時間: 2025-3-31 04:03
