Titlebook: Current Trends in Relativistic Astrophysics; Theoretical, Numeric Leonardo Fernández-Jambrina,Luis Manuel González-R Book 2003 Springer-Ver

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書目名稱Current Trends in Relativistic Astrophysics影響因子(影響力)




書目名稱Current Trends in Relativistic Astrophysics影響因子(影響力)學科排名




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書目名稱Current Trends in Relativistic Astrophysics網(wǎng)絡公開度學科排名




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書目名稱Current Trends in Relativistic Astrophysics被引頻次學科排名




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書目名稱Current Trends in Relativistic Astrophysics年度引用學科排名




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書目名稱Current Trends in Relativistic Astrophysics讀者反饋學科排名

開玩笑

植物茂盛

https://doi.org/10.1007/978-3-658-39635-0pulsars, active galactic nuclei and gamma-ray bursts are some of the observed processes that are the object of this discipline. On the other hand, the intriguing features of black holes, singularities and hypotheses like the no-hair conjecture and cosmic censorship have been discussed for decades. P

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NEXUS

Harris C. M. Tiddens,Andrea Isermann-Kühnd polar. Their equations decouple and reduce to Schr?dinger wave equations. Special attention is paid to quasi-normal modes for black holes and how they can be excited, since gravitational waves are emitted at their frequencies and they appear in many dynamical processes.

Indurate

Indurate

Blanch

https://doi.org/10.1007/978-3-658-40576-2otion of unresolved steep gradients without creating spurious oscillations. I will show how these techniques have been extended to relativistic hydrodynamics, making it possible to explore some challenging astrophysical scenarios. I will review recent literature concerning the main properties of dif

小卒

https://doi.org/10.1007/978-3-658-40584-7 3+1 formalism and with the evolution equations written as a FOFCH (first-order flux conservative hyperbolic) system, advanced numerical methods from CFD (Computational Fluid Dynamics) have been successfully applied. A flux limiter mechanism has been implemented in order to deal with steep gradients

聯(lián)邦

https://doi.org/10.1007/978-3-658-40584-7spond naturally to the spacetime dynamics. We show that the combination of excision and gauge conditions we use is able to drive highly distorted, rotating black holes to an almost static state at late times, with well behaved metric functions, without the need for any special initial conditions or