Molecular cloud

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A molecular cloud is a type of interstellar cloud whose density and size permits the formation of molecules, most commonly molecular hydrogen (H₂).

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.<ref>Craig Kulesa. Overview: Molecular Astrophysics and Star Formation. Research Projects. Retrieved on September 7, 2005.</ref>

1 Occurrence
2 Types of Molecular Cloud
3 Processes
- 3.1 Star Formation
- 3.2 Physics
4 References

[edit] Occurrence

Within our own Galaxy molecular gas accounts for less than one percent of the volume of the interstellar medium )(ISM), yet it is also the densest part of the medium comprising roughly one-half of the total gas mass interior to the Sun's galactic orbit. The bulk of the molecular gas is contained in a molecular ring between 3.5 to 7.5 kiloparsecs from the centre of the galaxy (the Sun is about 8.5 kiloparces from the center).<ref name="ferriere2001">Ferriere, D. (2001). "The Interstellar Environment of our Galaxy.". Reviews of Modern Physics 73 (4): 1031-1066.</ref> Large scale carbon monoxide maps of the galaxy show that the position of this gas correlates with the spiral arms of the galaxy.<ref>Dame et al (1987). "A composite CO survey of the entire Milky Way". Astrophysical Journal 322: 706-720.</ref> That molecular gas occurs predominantly in the spiral arms argues that molecular clouds must form and dissociate on a timescale shorter than 10 million years - the time it takes for material to pass through the arm region.<ref name="williams2000">Williams, J. P.; Blitz, L.; McKee, C. F., (2000). "The Structure and Evolution of Molecular Clouds: from Clumps to Cores to the IMF". Protostars and Planets IV, 97, Tucson: University of Arizona Press.</ref>

Vertically, the molecular gas inhabits the narrow midplane of the galactic disc with a characteristic scale height of approximately 50–75 parsec, much thinner than the warm atomic (Z=130-400pc) and hot ionized (Z=1000pc) gaseous components of the ISM. <ref>Cox, D. 2005, The Three-Phase Interstellar Medium Revisited, Annual Reviews of Astronomy and Astrophysics, 43, 337-85</ref> The exception to the ionized gas distribution are HII regions which are bubbles of hot ionized gas created in molecular clouds by the intense radiation given off by young massive stars and as such they have approximately the same vertical distribution as the molecular gas.

This smooth distrubtion of molecular gas is averaged out over large distances, however the small scale distribution of the gas is highly irregular with most of it concentrated in discrete clouds and cloud complexes.<ref name="ferriere2001" />

[edit] Types of Molecular Cloud

[edit] Giant Molecular Clouds (GMCs)

Vast assemblages of molecular gas with masses of 10⁴–10⁶ times the mass of the sun are called Giant molecular clouds (GMC). The clouds can reach tens of parsec in diameter and have an average density of 10²–10³ particles per cubic centimetre (the average density in the solar vincinty is one particle per cubic centimetre). Substructure within these clouds is a complex pattern of filaments, sheets, bubbles, and irregular clumps.<ref name="williams2000" />

The densest parts of the filaments and clumps are called "molecular cores", whilst the densest molecular cores are, unsurprisingly, called "dense molecular cores" and have densities in excess of 10⁴–10⁶ particles per cubic centimeter. Observationally molecular cores are traced with carbon monoxide and dense cores are traced with ammonia. The concentration of dust within molecular cores is normally sufficient to block light from background stars such that they appear in silhouette as dark nebulae.<ref name="francesco2006">Di Francesco, J., et al (2006). "An Observational Perspective of Low-Mass Dense Cores I: Internal Physical and Chemical Properties". Protostars and Planets V.</ref>

GMCs are so large that "local" ones can cover a significant fraction of a constellation such that they are often referred to by the name of that constellation, e.g. the Orion Molecular Cloud (OMC) or the Taurus Molecular Cloud (TMC). These local GMCs are arrayed in a ring around the sun called the Gould Belt. <ref>Grenier (2004). "The Gould Belt, star formation, and the local interstellar medium". The Young Universe. Electronic preprint</ref>The most massive collection of molecular clouds in the galaxy, the Sagittarius B2 complex, forms a ring around the galactic centre at a radius of 120 parsec. The Sagittarius region is chemically rich and is often used as an exemplar by astronomers searching for new molecules in interstellar space.<ref>[http://www.mpifr-bonn.mpg.de/staff/epolehampton/thesis/node23.html Sagittarius B2 and its Line of Sight</ref>

[edit] Small Molecular Clouds

Main article: Bok globule

Isolated gravitationally bound small molecular clouds with masses less than a few hundred times the mass of the sun are called Bok globule. The densest parts of small molecular clouds are equivalent to the molecular cores found in GMCs and often included in the same studies.

[edit] High Latitude Diffuse Molecular Clouds

Main article: Infrared Cirrus

In 1984 IRAS identified a new type of diffuse molecular cloud.<ref>Low et al (1984). "Infrared cirrus - New components of the extended infrared emission". Astrophysical Journal 278: L19-L22.</ref> These were diffuse filamentary clouds that are visible at high galactic latitudes (looking out of the plain of the galactic disc). These clouds would have a typical density of 30 particles per cubic centimeter.<ref>Gillmon, K., and Shull, J.M. (2006). "Molecular Hydrogen in Infrared Cirrus". Astrophysical Journal 636: 908-915. </ref>

[edit] Processes

[edit] Star Formation

Main article: Star Formation

To our knowledge, the creation of newborn stars in the current Universe occurs exclusively within molecular clouds. This is a natural consequence of their low temperatures and high densities, and of the observed evidence that the large, star-forming clouds are confined to a large degree by their own gravity (like stars, planets, and galaxies) rather than external pressure (like clouds in the sky). The evidence comes from the fact that the "turbulent" velocities inferred from CO linewidth scale in the same manner as the orbital velocity (a virial relation).

[edit] Physics

The physics of molecular clouds are poorly understood and much debated. Their internal motions are governed by turbulence in a cold, magnetized gas, for which the turbulent motions are highly supersonic but comparable to the speeds of magnetic disturbances. This state is thought to lose energy rapidly, requiring either an overall collapse or a steady reinjection of energy. At the same time, the clouds are known to be disrupted by some process—most likely the effects of massive stars—before a significant fraction of their mass has become stars.

Molecular clouds, and especially "Giant" molecular clouds (GMCs), are often the home of astronomical masers.