scholarly journals Two‐Dimensional Multiangle, Multigroup Neutrino Radiation‐Hydrodynamic Simulations of Postbounce Supernova Cores

2008 ◽  
Vol 685 (2) ◽  
pp. 1069-1088 ◽  
Author(s):  
Christian D. Ott ◽  
Adam Burrows ◽  
Luc Dessart ◽  
Eli Livne
Keyword(s):  
Two Dimensional ◽  
Hydrodynamic Simulations ◽  
Neutrino Radiation

scholarly journals Systematic two-dimensional radiation-hydrodynamic simulations of super-Eddington accretion flow and outflow: Comparison with the slim disk model

2018 ◽  
Vol 70 (6) ◽  
Author(s):  
Takaaki Kitaki ◽  
Shin Mineshige ◽  
Ken Ohsuga ◽  
Tomohisa Kawashima
Keyword(s):  
Two Dimensional ◽  
Disk Model ◽  
Hydrodynamic Simulations ◽  
Accretion Flow

scholarly journals A numerical study of the interaction between two ejecta in the interplanetary medium: one- and two-dimensional hydrodynamic simulations

2004 ◽  
Vol 22 (10) ◽  
pp. 3741-3749 ◽  
Author(s):  
A. Gonzalez-Esparza ◽  
A. Santillán ◽  
J. Ferrer
Keyword(s):  
Hydrodynamic Model ◽  
Physical Mechanism ◽  
Interplanetary Medium ◽  
Numerical Study ◽  
Two Dimensions ◽  
Magnetic Clouds ◽  
The Sun ◽  
Two Dimensional ◽  
Hydrodynamic Simulations

Abstract. We studied the heliospheric evolution in one and two dimensions of the interaction between two ejecta-like disturbances beyond the critical point: a faster ejecta 2 overtaking a previously launched slower ejecta 1. The study is based on a hydrodynamic model using the ZEUS-3-D code. This model can be applied to those cases where the interaction occurs far away from the Sun and there is no merging (magnetic reconnection) between the two ejecta. The simulation shows that when the faster ejecta 2 overtakes ejecta 1 there is an interchange of momentum between the two ejecta, where the leading ejecta 1 accelerates and the tracking ejecta 2 decelerates. Both ejecta tend to arrive at 1AU having similar speeds, but with the front of ejecta 1 propagating faster than the front of ejecta 2. The momentum is transferred from ejecta 2 to ejecta 1 when the shock initially driven by ejecta 2 passes through ejecta 1. Eventually the two shock waves driven by the two ejecta merge together into a single stronger shock. The 2-D simulation shows that the evolution of the interaction can be very complex and there are very different signatures of the same event at different viewing angles; however, the transferring of momentum between the two ejecta follows the same physical mechanism described above. These results are in qualitative agreement with in-situ plasma observations of "multiple magnetic clouds" detected at 1AU.

GRB-SN CONNECTION: CENTRAL ENGINE OF LONG GRBs AND EXPLOSIVE NUCLEOSYNTHESIS

2011 ◽  
Vol 20 (10) ◽  
pp. 1975-1978 ◽  
Author(s):  
SHIGEHIRO NAGATAKI
Keyword(s):  
Numerical Simulations ◽  
Deposition Rate ◽  
Energy Deposition ◽  
Two Dimensional ◽  
Hydrodynamic Simulations ◽  
X Ray ◽  
Central Engine ◽  
Explosive Nucleosynthesis ◽  
General Relativistic ◽  
Energy Deposition Rate

I have developed two-dimensional general relativistic magnetohydrodynamic (GRMHD) code. I have performed numerical simulations of collapsars using these codes and realistic progenitor models. In the GRMHD simulation, it is shown that a jet is launched from the center of the progenitor. We also performed two-dimensional hydrodynamic simulations in the context of collapsar model to investigate the explosive nucleosynthesis happened there. It is found that the amount of 56 Ni is very sensitive to the energy deposition rate. This result means that the amount of synthesized 56 Ni can be little even if the total explosion energy is as large as 1052 erg. Thus, some GRBs can associate with faint supernovae. Thus we consider it is quite natural to detect no underlying supernova in some X-ray afterglows.

scholarly journals SUBGRID MODELLING IN DEPTH INTEGRATED FLOWS

1988 ◽  
Vol 1 (21) ◽  
pp. 35 ◽  
Author(s):  
P.A. Madsen ◽  
M. Rugbjerg ◽  
I.R. Warren
Keyword(s):  
Shear Stress ◽  
Large Scale ◽  
Eddy Viscosity ◽  
Grid Size ◽  
Coastal Engineering ◽  
Shear Stresses ◽  
Two Dimensional ◽  
Bottom Shear Stress ◽  
Hydrodynamic Simulations ◽  
Engineering Studies

Hydrodynamic simulations in coastal engineering studies are still most commonly carried out using two-dimensional vertically integrated mathematical models. As yet, threedimensional models are too expensive to be put into general use. However, the tendency with 2-D models is to use finer and finer resolution so that it becomes necessary to include approximations to some 3-D phenomena. It has been shown by many authors that simulations of large scale eddies can be quite realistic in 2-D models (c.f. Abbott et al. 1985). Basically there exists two different mechanisms of circulation generation. The first one is based on a balance between horizontally and grid-resolved momentum transfers and the bed resistance - i.e. a balance between the convective momentum terms and the bottom shear stress. The second one is due to momentum transfers that are not resolved at the grid scale but appears instead as horizontally distributed shear stresses. In many practical situations the circulations will be governed by the first mechanism. This is the case if the diameter of the circulation and the grid size is much larger than the water depth. In this situation the eddies are friction dominated so that the effect of sub-grid eddy viscosity is limited. In this case 2-D models are known to produce very realistic results and several comparisons with measurements have been reported in the literature.

One‐dimensional and Pseudo–Two‐dimensional Hydrodynamic Simulations of Solar X‐Ray Jets

2001 ◽  
Vol 550 (2) ◽  
pp. 1051-1063 ◽  
Author(s):  
Masumi Shimojo ◽  
Kazunari Shibata ◽  
Takaaki Yokoyama ◽  
Kuniko Hori
Keyword(s):  
Two Dimensional ◽  
Hydrodynamic Simulations ◽  
One Dimensional ◽  
X Ray

scholarly journals Theory, observation and experiment: stellar hydrodynamics

1997 ◽  
Vol 189 ◽  
pp. 389-394
Author(s):  
David Arnett
Keyword(s):  
Computer Simulations ◽  
Computer Technology ◽  
Stellar Evolution ◽  
Analytical Methods ◽  
Simulation Methods ◽  
Two Dimensional ◽  
Predictive Capability ◽  
Hydrodynamic Simulations ◽  
Critical Comparison ◽  
Numerical And Analytical Methods

Computer technology now allows two dimensional (2D) simulations, with complex microphysics, of stellar hydrodynamics and evolutionary sequences, and holds the promise for 3D. Careful validation of astrophysical methods, by laboratory experiment, by critical comparison of numerical and analytical methods, and by observation are necessary for the development of simulation methods with reliable predictive capability. Recent and surprising results from isotopic patterns in pre-solar grains, 2D hydrodynamic simulations of stellar evolution, and laser tests and computer simulations of Richtmeyer-Meshkov and Rayleigh-Taylor instabilities will be discussed, and related to stellar evolution and supernovae.

scholarly journals Nucleosynthesis in neutrino-driven, aspherical Population III supernovae

2011 ◽  
Vol 7 (S279) ◽  
pp. 237-240
Author(s):  
Shin-ichiro Fujimoto ◽  
Masa-aki Hashimoto ◽  
Masaomi Ono ◽  
Kei Kotake
Keyword(s):  
Nuclear Reaction ◽  
Atomic Number ◽  
Reaction Network ◽  
Explosion Energy ◽  
Two Dimensional ◽  
Post Processing ◽  
Hydrodynamic Simulations ◽  
Artificial Mixing ◽  
Spherical Models ◽  
Accretion Shock

AbstractWe investigate explosive nucleosynthesis during neutrino-driven, aspherical supernova (SN) explosion aided by standing accretion shock instability (SASI), based on two-dimensional hydrodynamic simulations of the explosion of 11, 15, 20, 25, 30 and 40M⊙ stars with zero metallicity. The magnitude and asymmetry of the explosion energy are estimated with simulations, for a given set of neutrino luminosities and temperatures, not as in the previous study in which the explosion is manually and spherically initiated by means of a thermal bomb or a piston and also some artificial mixing procedures are applied for the estimate of abundances of the SN ejecta.By post-processing calculations with a large nuclear reaction network, we have evaluated abundances and masses of ejecta from the aspherical SNe. We find that matter mixing induced via SASI is important for the abundant production of nuclei with atomic number ≥ 21, in particular Sc, which is underproduced in the spherical models without artificial mixing. We also find that the IMF-averaged abundances are similar to those observed in extremely metal poor stars. However, observed [K/Fe] cannot be reproduced with our aspherical SN models.

scholarly journals Supernova Ejecta Interacting with a Circumstellar Disk. I. Two-dimensional Radiation-hydrodynamic Simulations

2019 ◽  
Vol 887 (2) ◽  
pp. 249 ◽  
Author(s):  
Akihiro Suzuki ◽  
Takashi J. Moriya ◽  
Tomoya Takiwaki
Keyword(s):  
Circumstellar Disk ◽  
Two Dimensional ◽  
Hydrodynamic Simulations
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