Interstellar matter

Template:TOC-right Interstellar matter is all uncoalesced matter in the regions between stars. It is comprised of solid dust, neutral gas and ionized plasma.

The interstellar medium contains ionised elements (predominantly carbon, silicon and sulphur), neutral elements (most of which is hydrogen, helium, nitrogen, oxygen, neon and argon) and condensed dust grains (primarily aluminium, calcium magnesium, and iron). The lightest elements, hydrogen, helium and lithium, were formed during the Big Bang. Heavier elements were created within stars by nucleosynthesis before being ejected into interstellar space by stellar winds and supernova explosions.

The interstellar matter closer to our solar system includes matter created after the original nebula from which our sun was formed and is expected to be richer in heavier elements and neutron rich isotopes.

Interstellar matter coalesces to form stars.

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General Properties

Galaxies contains significant amounts of tenuous matter, unevenly distributed throughout interstellar space. It is composed of gas (atoms, molecules, ions, and electrons) and dust (tiny solid particles). Interstellar matter obscures, reddens and polarises of starlight by forming absorption lines in stellar spectra, and through other emission mechanisms (both over a continuum and at specific wavelengths).

Interstellar matter comprises a small percentage of the total mass of a galaxy, about 10 − 15 % of the total mass of the galactic disk of the Milky Way, and tends to concentrate near the galactic plane and along the spiral arms in spiral galaxies.

Approximately 50% of interstellar matter forms discrete clouds which occupy about 1 − 2 % of the interstellar volume.

Interstellar clouds

There are three types of interstellar clouds:

• Dark clouds - Essentially very cold molecular gas ranging in temperature from 10 − 20 K and block off the light from background stars;
• Diffuse clouds - Cold atomic gas at about 100 K, almost transparent to the background starlight. However, at a number of specific wavelengths they give rise to absorption lines;
• Translucent clouds - Composed of molecular and atomic gases and have intermediate visual extinctions.

Between the clouds there are three different forms of interstellar matter:

• warm (mostly neutral) atomic matter about 104 K,
• warm ionized matter about 104 K
• hot ionized matter about 106 K

Density

Interstellar matter is very thinly distributed, tenuous. In the region of the Sun it averages about 2.7 x 10⁻²⁴ g cm⁻³, ranging from about 1.5 x 10²⁶ g cm^-3 in the hot medium from approximately 2 x 10⁻²⁰ to 2 x 10⁻¹⁸ g cm⁻³ in the densest molecular regions. This is about the same as a single hydrogen atom per cubic centimetre or nearly 20 orders of magnitude below that of the Earth’s lower atmosphere.