Everything about Interstellar Cloud totally explained
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) (ie. 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
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 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.
Unexpected chemicals detected in interstellar clouds
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, large
organic molecules were observed in the spectra that
scientists wouldn't have expected to find under these conditions. The reactions needed to create them normally occur only at much higher temperatures and pressures. The fact that they were found indicates that these
chemical reactions in interstellar clouds take place faster than suspected. These reactions are studied in the
CRESU experiment.
High-velocity cloud
These interstellar clouds possess a velocity higher than can be explained by the rotation of the
Milky Way. By definition, these clouds must have a v
lsr greater then 90 km s
-1, where v
lsr is the local standard rest velocity. They are detected primarily in the
21 cm line of neutral
hydrogen, and typically have a lower portion of heavy elements than is normal for interstellar clouds in the Milky Way.
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.
High-velocity clouds are identified with an HVC prefix, as with
HVC 127-41-330.
Further Information
Get more info on 'Interstellar Cloud'.
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