Latest Interstellar medium Stories
An international team of scientists led by University of Hawai'i at Mānoa Professor Ralf I. Kaiser, Alexander M. Mebel of Florida International University, and Alexander Tielens of Leiden Observatory in the Netherlands, discovered a novel chemical route to form polycyclic aromatic hydrocarbons (PAHs) – complex organic molecules such as naphthalene carrying fused benzene rings – in ultra-cold regions of interstellar space.
The constellation Cygnus, now visible in the western sky as twilight deepens after sunset, hosts one of our galaxy's richest-known stellar construction zones.
The discovery of 13 diffuse interstellar bands with the longest wavelengths to date could someday solve a 90-year-old mystery.
In the Oct. 26 issue of the journal Nature, astronomers report that organic compounds of unexpected complexity exist throughout the Universe.
Sino-German research group draws a new map at the Urumqi radio telescope and discovers two supernova remnants.
In a paper to be published in the April 10, 2011, issue of The Astrophysical Journal, scientists on NASA's Interstellar Boundary Explorer (IBEX) mission, including lead author Nathan Schwadron and others from the University of New Hampshire, isolate and resolve the mysterious "ribbon" of energy and particles the spacecraft discovered in the heliosphere â€“ the huge bubble that surrounds our solar system and protects us from galactic cosmic rays.
Pattern of X-ray 'stripes' in supernova remnant could explain how cosmic rays are produced.
Just as some drivers obey the speed limit while others treat every road as if it were the Autobahn, some stars move through space faster than others.
PASADENA, Calif., Dec. 13, 2010 /PRNewswire-USNewswire/ -- The 33-year odyssey of NASA's Voyager 1 spacecraft has reached a distant point at the edge of our solar system where there is no outward motion of solar wind.
The 33-year odyssey of NASA's Voyager 1 spacecraft has reached a distant point at the edge of our solar system where there is no outward motion of solar wind.
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...
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