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Interstellar cloud

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Title: Interstellar cloud  
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Subject: G-Cloud, Molecular cloud, Cyclopropenylidene, Glossary of astronomy, Smith's Cloud
Collection: Articles Containing Video Clips, Cosmic Dust, Intergalactic Media, Interstellar Media, Nebulae
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Interstellar cloud

Small part of the emission nebula NGC 6357. It glows with the characteristic red of an H II region.[1]

Interstellar cloud is the generic name given to an accumulation of gas, plasma and dust in our and other galaxies. Put differently, an interstellar cloud is a denser-than-average region of the interstellar medium. Depending on the density, size and temperature of a given cloud, the hydrogen in it can be neutral (H I regions), ionized (H II regions) (i.e. a plasma), or molecular (molecular clouds). Neutral and ionized clouds are sometimes also called diffuse clouds, while molecular clouds are sometimes also referred to as dense clouds.


  • Chemical compositions 1
  • Unexpected chemicals detected in interstellar clouds 2
  • High-velocity cloud 3
  • See also 4
  • References 5
  • External links 6

Chemical compositions

Analyzing 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 electromagnetic radiation which are characteristic of certain molecules' spectra. Some interstellar clouds are cold and tend to give out EM radiation of large wavelengths. We can produce a map of the abundance of these molecules to produce an understanding of the varying composition of the clouds. In hot clouds, there are often ions of many elements, whose spectra can be seen in visible and ultraviolet light.

Radio telescopes can also scan over the frequencies from one point in the map, recording the intensities of each type of molecule. Peaks of frequencies mean that an abundance of that molecule or atom is present in the cloud. The height of the peak is proportional to the relative percentage that it makes up.[2]

Unexpected chemicals detected in interstellar clouds

Dive into the Lagoon Nebula

Until recently the rates of reactions in interstellar clouds were expected to be very slow, with minimal products being produced due to the low temperature and density of the clouds. However,

External links

  1. ^ "Carved by Massive Stars". ESO Picture of the Week. Retrieved 13 September 2013. 
  2. ^ Project Leader Dr. Lochner (November 2009). "Spectra and What Scientists Can Learn From Them". Goddard Space Flight Center, NASA. Retrieved 12 February 2010. 
  3. ^ Charles Blue (October 2001). "Scientists Toast the Discovery of Vinyl Alcohol in Interstellar Space". National Radio Astronomy Observatory. Retrieved 9 February 2010. 
  4. ^ Knauth, D., Federman, S. and Lambert, D. Newly Synthesized Lithium in the Interstellar Medium Nature 405 (2000): 656-658. Print.
  5. ^ Navarro, J. F., Frenk, C. S., & White, S. D. M. 1995, Monthly Notices of the Royal Astronomical Society, 275, 720
  6. ^ "Dark Matter- More Than Meets the Eye". NASA. Retrieved 12 February 2010. 


See also

High-velocity clouds are identified with an HVC prefix, as with HVC 127-41-330.

Theories intended to explain these unusual clouds include materials left over from the formation of our galaxy, or tidally-displaced matter drawn away from other galaxies or members of the Local Group. An example of the latter is the Magellanic Stream. To narrow down the origin of these clouds, a better understanding of their distances and metallicity is needed.

These interstellar clouds possess a velocity higher than can be explained by the rotation of the Milky Way.[5] By definition, these clouds must have a vlsr greater than 90 km s−1, where vlsr is the local standard rest velocity. They are detected primarily in the 21 cm line of neutral hydrogen,[6] and typically have a lower portion of heavy elements than is normal for interstellar clouds in the Milky Way.

Reflection nebula IRAS 10082-5647 taken by Hubble Space Telescope.

High-velocity cloud

Interstellar clouds also provide a medium to study the presence and proportions of metals in space. The presence and ratios of these elements may help develop theories on the means of their production, especially when their proportions are inconsistent with those expected to arise from stars as a result of fusion and thereby suggest alternate means, such as cosmic ray spallation.[4]

. CRESU experiment These reactions are studied in the [3]

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