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Research Gallery
Computational Astrophysics (formerly CFDMHD)
Formation and Evolution of Protoplanetary and Circumplanetary Disks with Antares ThreeDimensional Global Hydrodynamic Simulations Figure: Example of a nestedgrid mesh refinement (NMR) run of a global protoplanetary disk with an embedded circumplanetary disk surrounding a 0.05Jupitermass planet at 5.2 AU from the star at ...(more) 

Cotribution analysis of molecular line of a disk the plot visualizes the contribution of the specific transition of the molecule from a certain observing angle ...(more) 

Formation of Isothermal Circumplanetary Disks with ThreeDimensional Global Simulations for SubNeptuneMass Protoplanets In the bottom panels, square sections of surface density simulated with Antares are shown centered at the locations of protoplanets. The surface density is obtained by vertical integration over z ...(more) 

A Selfconsistent Model for Super/subluminal Motions and Particle Acceleration in the M87 Jet Distribution of the physical quantities along the jet propagation axis. We perform special relativistic MHD simulations in a cylindrical 1.5dimensional pproximation. Our model reproduces a paired super/subluminal knot motions, taken ...(more) 

HYDRODYNAMICAL SIMULATIONS OF THE BARRED SPIRAL GALAXY NGC 1097 A comparison between the numerical simulation result and the observation of NGC 1097. Left panel: The projected surface density distribution of the simulation result. Middle panel: Optical image of NGC ...(more) 

Microejections in stardisk resistive magnetohydrodynamic simulations In simulations of a stardisk system in the closest vicinity of a star, we obtain very fast, light ejecta of matter. Those microejections are of small mass and angular momentum ...(more) 

Selfgravitational force calculation of infinitely thin gaseous disks The numerical solutions of a D2 disk for N=1024, the profiles are surface density (lefttop), the xdirectional force (righttop), the ydirectional force(leftbottom), and radial force(rightbottom). ...(more) 

Probing Substellar Companions of Asymptotic Giant Branch Stars through Spirals and Arcs Three dimensional hydrodynamical simulations show that the substellar mass objects produce detectable signatures, corresponding to density contrasts of 10200 % and arm separations of 10400 AU at 100 AU distance, ...(more) 

Collimated fast winds in Preplanetary Nebulae Simulations of our CFW models from 1 to 6, at the age of ~160 yr. Parts (a), (c), (e), (g), (i), and (k) show the number density of hydrogen nuclei ...(more) 

Magnetospheric Accretion and Ejection of Matter in Resistive MHD Simulations In numerical simulations of the stardisk system, after the relaxation, the disk is truncated at the truncation radius R_t. Position of the R_t is close to the line of balance ...(more) 

Gravitationally Induced Density Wake of a Circularly Orbiting Object As an Interpretative Framework of Ubiquitous Spirals and Arcs The above figures show the density enhancement of the spiralonion shell shape (a) in the equatorial plane, (b) in a meridional plane, and (c) as a function of the distance ...(more) 

The Effect of Bars and Transient Spirals on the Vertical Heating in Disk Galaxies The left panel corresponds to the particle image showing the face on and two edge on views of an initially axisymmetric disk. The right panel shows the formation of a ...(more) 

Impact of Type Ia Supernova Ejecta on a Helium Star Binary Companion Observations of SNIa rates as a function of redshift suggest the existence of a short delay time population of 100 Myr and a long delay time population of 34 Gyr. ...(more) 

On the Orbital Evolution of a Jovian Planet Embedded in a SelfGravitating Disk Our simulations indicate that in the study of the runaway (type III) migration, it is important to carry out a fully self consistent treatment of the gravitational interaction between the ...(more) 

Hydrodynamical Simulations of the Barred Spiral Galaxy NGC 6782 Numerical calculations reveal that the striking features in NGC 6782 can be reproduced provided that the gas flow is governed by the gravitational potential associated with a slowly rotating strong ...(more) 

Simulations of winds Simulations of winds of terminal speed of 300 km/s (~3Va) and ambient densities 10E20 g/cm^3. The results are plotted on fourpanels to illustrate selected time frames of 100, 400, 700, ...(more) 