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Density (top) and temperature (bottom) snapshots from an idealized hydro-simulation of the circum-galactic medium of a Milky-Way-like galaxy. Note the outskirts (>70 kpc) are cool and free-falling, while the inner region is hot and pressure-supported.

The figure shows a radiative-hydrodynamic simulation of a dusty cloud irradiated by a quasar (located at r = 0). Radiation pressure is set to be the dominant pressure source. Left panel shows the initial conditions, while the right panel shows the cloud 10^4 years after exposure to the quasar radiation. A quasi-static density gradient develops at

Cataclysmic Variable stars (CVs) are binary star systems where an ultra-dense star (a white dwarf) pulls material off of its companion star, steadily consuming it over time. Depending on how strong the magnetic field strength of the white dwarf is, this material might be channelled down onto the surface of the white dwarf via magnetic

Massive stars end their lives in powerful explosions (supernovae) that span a wide range of energies and properties. The most powerful of these are the appropriately named Superluminous Supernovae (SLSNe). As SLSNe are so bright and energetic, we can see them out to great distances in the universe, and they could prove to be very

Gallery of Andromeda Star Clusters from Andromeda Project Catalog

Hubble Image Mosaic of Andromeda, based on PHAT survey data. This image, captured with the NASA/ESA Hubble Space Telescope, is the largest and sharpest image ever taken of the Andromeda galaxy, otherwise known as M31. You would need more than 600 HD television screens to display the whole image. It is the biggest Hubble image

“Hot Jupiters” are Jupiter-like planets with orbits close to their host star. Their origins are debated, and some young planetary system may even host multiple Hot Jupiters. Here, we investigate a planetary system of two Hot Jupiters orbiting a Sun-like star. The system is born on the edge of instability, and over time, the planets’

In late 2015, LIGO discovered gravitational waves emitted by two black holes (each with a mass of about 30 times that of our Sun) that spiraled together and merged about 1.5 billion years ago. Astrophysicists are now debating which is the most likely mechanism that can bring two black holes like those observed so close

Here we show the evolution of a Milky Way-like galaxy over time. The top row shows the galaxy as it would appear today, the middle 3.5 billion years ago, and the bottom almost 10 billion years ago. Columns give different views of the same snapshot in time, leftmost is the mock view through the Hubble

A screenshot from Firefly, an interactive, web-based, and publicly available particle visualization platform created by Aaron Geller and Alex Gurvich. Shown here is a snapshot in time from a simulation of a Milky Way-like galaxy with the stars in blue, the gas in red, and the dark matter in yellow. In the real universe the gas

Marked on this ALMA image are the locations and orientations of 11 gas outflows, which look like the bipolar lobes made by young protostars. These outflows are all within about 3 light-years of our galaxy’s supermassive black hole, marked with a star. Outflow #1 has the most obvious structure; the rest don’t show up well

This collection of images shows gas swirling around the same galaxy in several different ways. Taken together, the columns create a time-lapse projection. The top row shows the density of gas in the galaxy at a given time: in these panels, the brightest areas show where gas is most densely concentrated. In the middle row,