Molecular cloud

Within a few million years the light from bright stars will have boiled away this molecular cloud of gas and dust. The cloud has broken off from the Carina Nebula. Newly formed stars are visible nearby, their images reddened by blue light being preferentially scattered by the pervasive dust. This image spans about two light-years and was taken by the Hubble Space Telescope in 1999.

A molecular cloud, sometimes called a stellar nursery (if star formation is occurring within), is a type of interstellar cloud, the density and size of which permit the formation of molecules, most commonly molecular hydrogen (H2). This is in contrast to other areas of the interstellar medium that contain predominantly ionized gas.

Molecular hydrogen is difficult to detect by infrared and radio observations, so the molecule most often used to determine the presence of H2 is carbon monoxide (CO). The ratio between CO luminosity and H2 mass is thought to be constant, although there are reasons to doubt this assumption in observations of some other galaxies.[1]

Within molecular clouds are regions with higher density, where lots of dust and gas cores reside, called clumps. These clumps are the beginning of star formation, if gravity can overcome the high density and force the dust and gas to collapse.[2]

Occurrence

Molecular cloud Barnard 68, about 500 ly distant and 0.5 ly in diameter.

Within the Milky Way, molecular gas clouds account 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 half of the total gas mass interior to the Sun's galactic orbit. The bulk of the molecular gas is contained in a ring between 3.5 and 7.5 kiloparsecs (11,000 and 24,000 light-years) from the center of the Milky Way (the Sun is about 8.5 kiloparsecs from the center).[3] Large scale CO maps of the galaxy show that the position of this gas correlates with the spiral arms of the galaxy.[4] That molecular gas occurs predominantly in the spiral arms suggests 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.[5]

Circinus molecular cloud has a mass around 250,000 times that of the Sun.[6]

Vertically to the plane of the galaxy, the molecular gas inhabits the narrow midplane of the galactic disc with a characteristic scale height, Z, of approximately 50 to 75 parsecs, much thinner than the warm atomic (Z from 130 to 400 parsecs) and warm ionized (Z around 1000 parsecs) gaseous components of the ISM.[7] The exception to the ionized-gas distribution are H II 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 distribution 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.[3]

Types of molecular cloud

Giant molecular clouds

Part of the Taurus Molecular Cloud.[8]

A vast assemblage of molecular gas with a mass of approximately 103 to 107 times the mass of the Sun[9] is called a giant molecular cloud (GMC). GMCs are around 15 to 600 light-years in diameter (5 to 200 parsecs).[9] Whereas the average density in the solar vicinity is one particle per cubic centimetre, the average density of a GMC is a hundred to a thousand times as great. Although the Sun is much more dense than a GMC, the volume of a GMC is so great that it contains much more mass than the Sun. The substructure of a GMC is a complex pattern of filaments, sheets, bubbles, and irregular clumps.[5]

The densest parts of the filaments and clumps are called "molecular cores", while the densest molecular cores are called "dense molecular cores" and have densities in excess of 104 to 106 particles per cubic centimeter. Observationally, typical molecular cores are traced with CO and dense molecular cores are traced with ammonia. The concentration of dust within molecular cores is normally sufficient to block light from background stars so that they appear in silhouette as dark nebulae.[10]

GMCs are so large that "local" ones can cover a significant fraction of a constellation; thus 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 in the neighborhood of the Sun coinciding with the Gould Belt.[11] The most massive collection of molecular clouds in the galaxy forms an asymmetrical ring about the galactic center at a radius of 120 parsecs; the largest component of this ring is the Sagittarius B2 complex. The Sagittarius region is chemically rich and is often used as an exemplar by astronomers searching for new molecules in interstellar space.[12]

Distribution of molecular gas in 30 merging galaxies.[13]

Small molecular clouds

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

High-latitude diffuse molecular clouds

In 1984 IRAS identified a new type of diffuse molecular cloud.[14] These were diffuse filamentary clouds that are visible at high galactic latitudes. These clouds have a typical density of 30 particles per cubic centimeter.[15]

Processes

Young stars in and around molecular cloud Cepheus B. Radiation from one bright, massive star is destroying the cloud (from top to bottom in this image) while simultaneously triggering the formation of new stars.[16]

Star formation

The formation of stars occurs exclusively within molecular clouds. This is a natural consequence of their low temperatures and high densities, because the gravitational force acting to collapse the cloud must exceed the internal pressures that are acting "outward" to prevent a collapse. There is 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 by external pressure. 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).

Physics

The Serpens South star cluster is embedded in a filamentary molecular cloud, seen as a dark ribbon passing vertically through the cluster. This cloud has served as a testbed for studies of molecular cloud stability.[17]

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 GMCs, are often the home of astronomical masers.

See also

References

  1. ↑ Craig Kulesa. "Overview: Molecular Astrophysics and Star Formation". Research Projects. Retrieved September 7, 2005.
  2. ↑ Astronomy. https://d3bxy9euw4e147.cloudfront.net/oscms-prodcms/media/documents/Astronomy-Draft-20160817.pdf: Rice University. 2016. p. 761. ISBN 1938168283 – via Open Stax.
  3. 1 2 Ferriere, D. (2001). "The Interstellar Environment of our Galaxy". Reviews of Modern Physics. 73 (4): 1031–1066. Bibcode:2001RvMP...73.1031F. arXiv:astro-ph/0106359 Freely accessible. doi:10.1103/RevModPhys.73.1031.
  4. ↑ Dame; et al. (1987). "A composite CO survey of the entire Milky Way". Astrophysical Journal. 322: 706–720. Bibcode:1987ApJ...322..706D. doi:10.1086/165766.
  5. 1 2 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. Tucson: University of Arizona Press. p. 97. arXiv:astro-ph/9902246 Freely accessible.
  6. ↑ "Violent birth announcement from an infant star". ESA/Hubble Picture of the Week. Retrieved 27 May 2014.
  7. ↑ Cox, D. (2005). "The Three-Phase Interstellar Medium Revisited". Annual Review of Astronomy and Astrophysics. 43: 337–385. Bibcode:2005ARA&A..43..337C. doi:10.1146/annurev.astro.43.072103.150615.
  8. ↑ "APEX Turns its Eye to Dark Clouds in Taurus". ESO Press Release. Retrieved 17 February 2012.
  9. 1 2 See, e.g. Table 1 and the Appendix of Murray, N. (2011). "Star Formation Efficiencies and Lifetimes of Giant Molecular Clouds in the Milky Way". The Astrophysical Journal. 729 (2): 133. Bibcode:2011ApJ...729..133M. arXiv:1007.3270 Freely accessible. doi:10.1088/0004-637X/729/2/133.
  10. ↑ Di Francesco, J.; et al. (2006). "An Observational Perspective of Low-Mass Dense Cores I: Internal Physical and Chemical Properties". Protostars and Planets V. arXiv:astro-ph/0602379 Freely accessible.
  11. ↑ Grenier (2004). "The Gould Belt, star formation, and the local interstellar medium". The Young Universe. arXiv:astro-ph/0409096 Freely accessible. Electronic preprint
  12. ↑ Sagittarius B2 and its Line of Sight
  13. ↑ "Violent Origins of Disc Galaxies Probed by ALMA". www.eso.org. European Southern Observatory. Retrieved 17 September 2014.
  14. ↑ Low; et al. (1984). "Infrared cirrus – New components of the extended infrared emission". Astrophysical Journal. 278: L19. Bibcode:1984ApJ...278L..19L. doi:10.1086/184213.
  15. ↑ Gillmon, K. & Shull, J.M. (2006). "Molecular Hydrogen in Infrared Cirrus". Astrophysical Journal. 636 (2): 908–915. Bibcode:2006ApJ...636..908G. arXiv:astro-ph/0507587 Freely accessible. doi:10.1086/498055.
  16. ↑ "Chandra :: Photo Album :: Cepheus B  :: August 12, 2009".
  17. ↑ Friesen, R. K.; Bourke, T. L.; Francesco, J. Di; Gutermuth, R.; Myers, P. C. (2016). "THE FRAGMENTATION AND STABILITY OF HIERARCHICAL STRUCTURE IN SERPENS SOUTH". The Astrophysical Journal. 833 (2): 204. ISSN 1538-4357. doi:10.3847/1538-4357/833/2/204.
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