Exoplanet GSC 6214-210 b
Image of the planetary-mass companion GSC 6214-210 b (bottom) and its host star (top). (Credit: Ireland, M. J. et al 2011, ApJ, 726, 113)
Image of the planetary-mass companion GSC 6214-210 b (bottom) and its host star (top). (Credit: Ireland, M. J. et al 2011, ApJ, 726, 113)
Image of the planetary-mass companion VHS 1256-1257 b (bottom right) and its host star (center). (Credit: Gauza, B. et al 2015, MNRAS, 452, 1677-1683)
A Hubble Space Telescope view of the field that CEERS will survey. This field has been imaged by several surveys with Hubble, including AEGIS and CANDELS. A larger version (133Mb) of this image is available; click here to access. (Credit: Anton Koekemoer/STScI)
Artist’s concept of a view from within the exocomet system KIC 3542116. (Credit: Danielle Futselaar)
Evolution of the temperature and density structure in the protostellar accretion phase after the protostar formation. The rapid accretion of dense gas cloud (white contour) constricts an expansion of the photoionized region (red) which is possible to shut off the gas accretion. (Credit: Takashi Hosokawa)
Gas density distribution around the newborn protostar. The left-to-right supersonic gas motion results in the non-spherical, compressed density structure. (Credit: Shingo Hirano)
Projected density distributions of dark matter (background and top panel) and gas (bottom three panels) components when the massive star forms. The stellar cradle is extremely asymmetrical as a wide, wedge-shaped structure (middle panel) due to the initial supersonic gas motions left over from the Big Bang. The circle in the right panel indicates the gravitationally unstable region with mass of 26,000 solar-masses. (Credit: Shingo Hirano)
This image shows several of the binaries from this study, each orbiting around its center of mass, which is marked by an ‘x.’ Colors indicate surface temperatures, from warmest to coolest: gold, red, magenta, or blue. The background image is a map of the entire sky visible from Hawaii and a silhouette of Mauna Kea (home of Keck Observatory and the Canada-France-Hawaii Telescope, where this study was conducted over the past decade). Each binary is shown roughly where it is located in the night sky.
In this second artist's impression a huge sphere in the center of a galaxy is shown after a star has collided with it. Enormous amounts of heat and a dramatic increase in the brightness of the sphere are generated by this event. The lack of observation of such flares from the center of galaxies means that this hypothetical scenario is almost completely ruled out. (Mark A. Garlick/CfA)
This is the first in a sequence of two artist's impressions that shows a huge, massive sphere in the center of a galaxy, rather than a supermassive black hole. Here a star moves towards and then smashes into the hard surface of the sphere, flinging out debris. The impact heats up the site of the collision. (Mark A. Garlick/CfA)