Research Gallery

Image of the black hole in M87, obtained by the Event Horizon Telescope Collaboration. (...more)

The image shows the density distribution of a hypernova. An energetic explosion driven by both jets and disk winds leads to a large scale asymmetry in SN ejecta. (...more)

Very Large Array radio image of a single millisecond duration burst known as FRB 121102 (a,b). This is the first localization of an FRB, conclusively showing an extragalactic origin. The (...more)

AMR is used to resolve the finest structures in a hydro simulations. (...more)

The 3D CASTRO simulation shows that many fluid instabilities occur during a PSN explosion. (...more)

The image shows the density structure of colliding shells ejected by a massive star before it dies. Such collisions can easily convert the kinetic energy of ejecta into thermal radiation. (...more)

This image is a slice through the interior of a supermassive star of 55,500 solar masses along the axis of symmetry. It shows the inner helium core in which nuclear (...more)

Astrophysicist Ken Chen ran simulations on supercomputers to better understand the physical conditions that create superluminious supernova. (...more)

Distribution of the bulk velocity relative to the speed of light is shown as a function of the de-projected distance (normalized by r_s) from the core of the relativistic jet (...more)

VLBA total intensity map of the M87 jet at 43 GHz (2-a), showing the synchrotron radiation of relativistic electrons. A hollow, edge-brightened emission of the jet up to ~ 500 (...more)

Accretion geometry of disks for LLAGN corresponding to low rate of mass accretion. (...more)

Accretion geometry of disks for high luminosity AGN corresponding to high rates of mass accretion. (...more)

Luminosity evolution of pulsar outer magnetospheric accelerators as a function of neutron star spin down luminosity. Two extreme chemical compositions of the neutron star envelopes are considered. The red curves (...more)

Schematic picture (side view) of a pulsar magnetosphere. The filled circle on the left denotes the neutron star, which rotates along the vertical axis (dash-dotted line) with angular frequency "Omega". (...more)

Accretion geometry of disks for LLAGN (upper panel) and high luminosity AGN (lower panel) corresponding to high and low rates of mass accretion respectively. (Liu & Taam 2009, ApJ, 707, (...more)

Prototype of Graphitic Core for Two-Fluid Molten-Salt Heat-Exchanger (...more)

Figure 5 of "Pulsar Outer-gap Electrodynamics: Hardening of Spectral Shape in the Trailing Peak in Gamma-ray Light Curve", Kouichi Hirotani, Astrophys. J. 733, Letters 49-53 (2011). (...more)

Figure 15 of "Observations of the Crab pulsar above 25 GeV with the MAGIC I telescope", Aleksic et al. ApJ 742, 43 (2011) (...more)

Figure 2 of "Death Line of Gamma-ray Pulsars with Outer Gaps", Ren-Bo Wang and Kouichi Hirotani, ApJ 736, 127 (2011). (...more)

Monolithic collapse of a weakly magnetized cloud to form black holes. The red circle indicates the expansion wave, and the blue curves are the magnetic field lines. The left panel (...more)

Outer gap model of the emission mechanism from neutron stars (Takata et al, 2007, in press) (...more)