Latest Interstellar medium Stories
Scientists have for the first time detected a carbon-bearing molecule with a "branched" structure in interstellar space.
Once every 50 years, more or less, a massive star explodes somewhere in the Milky Way. The resulting blast is terrifyingly powerful, pumping out more energy in a split second than the sun emits in a million years. At its peak, a supernova can outshine the entire Milky Way.
From ancient, dying stars to our toothbrushes, the chemical element fluorine which is used in toothpaste was formed in stars of the same type as our sun billions of years ago, scientists from Lund University in Sweden believe.
Newly-created maps of the material located between the stars in the Milky Way could help astronomers solve a nearly century-long mystery involving stardust, according to a new study published in the August 15 edition of the journal Science.
Researchers at Harvard-Smithsonian Center for Astrophysics finger silicon-capped hydrocarbons as possible source of mysterious "diffuse interstellar bands."
For decades, scientists have been debating over a fog of low-energy X-rays that has been observed over the entire sky. An international group of scientists has used a NASA-funded instrument to resolve this debate.
The region in space around a planetary nebula is filled with harsh radiation. Yet despite this hostile environment, the area is seeded with a molecule essential to the formation of water.
Using a laser beam 60,000 billion times more powerful than a typical laser pointer, researchers have recreated a small scale supernova and revealed that cosmic turbulence may have boosted magnetic fields to the power seen in interstellar space.
A team of scientists at NASA's Ames Research Center has successfully reproduced, right here on Earth, the processes that occur in the atmosphere of a red giant star and lead to the formation of planet-forming interstellar dust.
Our Galaxy's magnetic field is revealed in a new image from ESA's Planck satellite. This image was compiled from the first all-sky observations of 'polarised' light emitted by interstellar dust in the Milky Way.
UV Astronomy -- UV astronomy is the branch of astronomy and astrophysics which deals with objects visible in ultraviolet (UV) radiation. UV radiation ranges approximatively from 10nm (extreme UV) to 380nm (near UV). Ultraviolet line spectrum measurements are used to discern the chemical composition, densities, and temperatures of interstellar medium, and the temperature and composition of hot young stars. UV observations can also provide essential information about the evolution of...
Molecular Cloud -- Molecular clouds are interstellar nebulae that have a density and size sufficient to permit the formation of H2, molecular hydrogen. However, this molecule is difficult to detect, and the molecule most used to trace the H2 is CO (carbon monoxide). The ratio between CO luminosity and H2 mass is roughly constant, although there are reasons to doubt this assumption in observations of some other galaxies. In the Milky Way, molecular clouds account for roughly one-half...
Interstellar Cloud -- Interstellar cloud is the generic name given to accumulations of gas and dust in our galaxy. Depending on the density, size and temperature of a given cloud, the hydrogen in it can be neutral (HI clouds) or molecular (molecular clouds). Chemical compositions Analysing the composition of interstellar clouds is achieved by studying electromagnetic radiation that we receive from them. Large radio telescopes scan the intensity in the sky of particular frequencies of...
Heliopause -- The heliopause is the boundary where our Sun's solar wind is stopped by the interstellar medium. The solar wind blows a "bubble" in the interstellar medium (the rareified hydrogen and helium gas that permeates the galaxy). The point where the solar wind's strength is no longer great enough to push back the interstellar medium is known as the heliopause, and is often considered to be the outer "border" of the solar system. The distance to the heliopause is not precisely...
Emission Nebula -- In astronomy, emission nebulae are clouds of ionized gas, emitting light of various colors. The most common source for ionization are high-energy photons emitted from a nearby young, hot star. Usually, a young star will ionize part of the same cloud from which it was born. Only big, hot stars can release the amount of energy required to ionize a significant part of a cloud. Often, an entire cluster of young stars is doing the work. The nebula's color depends on...
- One of a pair of round metal cymbals attached to the fingers and struck together for rhythm and percussion in belly dancing.