搜索结果: 1-13 共查到“天文学 SPH”相关记录13条 . 查询时间(0.062 秒)
Size–frequency distributions of fragments from SPH/N-body simulations of asteroid impacts: Comparison with observed asteroid families
Asteroids Collisional physics Impact processes
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2015/12/25
We investigate the morphology of size–frequency distributions (SFDs) resulting from impacts into 100-km-diameter parent asteroids, represented by a suite of 161 SPH/N-body simulations conducted to stu...
Galaxy merger statistics and inferred bulge-to-disk ratios in cosmological SPH simulations
formation spiral elliptical
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2014/12/24
We construct merger trees for galaxies identified in a cosmological hydrodynamic simulation and use them to characterize predicted merger rates as a function of redshift, galaxy mass, and merger mass ...
Accretion, feedback and galaxy bimodality: a comparison of the GalICS semi-analytic model and cosmological SPH simulations
cooling fl ows evolution
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2014/12/23
We compare the galaxy population of a smoothed particle hydrodynamics (SPH) simulation to those predicted by the GalICS (Galaxies In Cosmological Simulations) N-body + semi-analytic model and a stripp...
Growth of galaxies in SPH simulations
Explore Galaxy formation. Smooth particle hydrodynamics The universe simulation Galactic gas Temperature history Galaxy star
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2014/12/9
We explore the growth of galaxies formed in self-consistent Smoothed Particle Hydrodynamic (SPH) cosmological simulations. In the first Chapter, we examine the temperature history of gas accreted by f...
平滑粒子流体动力学(SPH)数值模拟中的重子物理
流体数值模拟 重子物理 恒星形成
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2012/9/12
平滑流体动力学(SPH)数值模拟是我们研究星系形成与演化的一个重要工具。先介绍了SPH的基本原理和基本方程，然后以恒星形成、星系风反馈、AGN反馈和热传导为例，介绍了平滑流体动力学数值模拟中的重子物理及实施方法。这些模型在一定程度上都取得了成功，对更好地理解星系的形成和演化起到了促进作用。
Simulating the Common Envelope Phase of a Red Giant Using SPH and Uniform Grid Codes
Simulating Common Envelope Phase Red Giant Using SPH Uniform Grid Codes
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2011/10/21
We use three-dimensional hydrodynamical simulations to study the rapid infall phase of the common envelope interaction of a red giant branch star of mass equal to 0.88 \msun and a companion star of ma...
Mass Transfer in Binary Stars using SPH. I. Numerical Method
galaxies active - line formation - radiation mechanism general - scattering - X-rays general
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2010/11/12
We present new results from Monte Carlo calculations of the flux and equivalent width
(EW) of the Ni K fluorescent emission line in the toroidal X-ray reprocessor model of
Murphy & Yaqoob (2009, MN...
Mass Transfer in Binary Stars using SPH. II. Eccentric Binaries
binaries close — stars evolution — hydrodynamics — methods numerical
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2010/11/12
Despite numerous efforts to better understand binary star evolution, some aspects of it remain
poorly constrained. In particular, the evolution of eccentric binaries has remained elusive mainly becau...
The impact of numerical viscosity in SPH simulations of galaxy clusters
Cosmology and Extragalactic Astrophysics (astro-ph.CO)
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2011/1/6
A SPH code employing a time-dependent artificial viscosity scheme is used to construct a large set of N-body/SPH cluster simulations for studying the impact of artificial viscosity on the thermodynami...
Sph and radiative cooling
Sph radiative cooling
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2009/6/17
Sph and radiative cooling。
Sph simulations of early and late superhumps
Sph simulations superhumps
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2009/6/17
Sph simulations of early and late superhumps。
SPH with radiative transfer：method and applications
radiative transfer SPH
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2009/6/16
SPH with radiative transfer：method and applications。
3D sph simulations of giant herbig-haro flows and jet-cloud interactions in star formation regions
smoothed particle hydro-dynamics star formation regions
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2009/6/4
We review some recent results of three-dimensional smoothed particle hydro-dynamics (SPH) simulations of overdense, radiatively cooling jets in star formingregions. We discuss the structure and kinema...