associated molecular cloud
abr-e molekuli-ye âhazidé
Fr.: nuage moléculaire associé
A → molecular cloud that is physically or apparently related to a star formation region.
Central Molecular Zone (CMZ)
zonâr-e molekuli-ye markazi
Fr.: zone moléculaire centrale
A vast, turbulent region encircling the → Milky Way's nucleus that contains a large fraction of the → Galaxy's dense → molecular clouds and → star formation regions. Spanning -1 to +1.5 degrees of → Sgr A*, the CMZ is about 400 pc × 100 pc in size and contains at least 107→ solar masses of → giant molecular clouds, approximately 10% of the Galaxy's molecular gas. The gas in the CMZ is at higher temperature than typical giant molecular clouds and has high velocity dispersion reflecting the → turbulent nature of the gas in the area. Despite these extensive molecular reserves, the → star formation rate within the CMZ is actually lower than expected based on the analysis of nearby → star-forming regions in the quiescent → Galactic disk. A common assumption is that this is a result of the extreme conditions within the CMZ, where the density, pressure, temperature, → velocity dispersion and → radiation field are all significantly greater than elsewhere in the Milky Way (Clark et al. 2018, The Messenger 173, 22 and references therein).
Fr.: molécule de méthylidine
Fr.: molécule CN
The simplest molecule formed by the → cyano radical. The CN molecule is of considerable astrophysical importance, since many of its transition lines/bands are observed in various astronomical objects: interstellar medium, comets, various stars such as late-type F and G-dwarfs, and late-type giants. CN was the second interstellar molecule, after → CH (methylidine), to be identified; toward the bright star → Zeta Ophiuchi at ultraviolet wavelengths (A. McKellar, 1940 ASP Conf. Ser. 52, 187). CN was also one of the earliest molecules to be detected in other galaxies (Henkel et al. 1988, A&A 201L, 23).
Fr.: molécule complexe
A molecule in the → interstellar medium comprising at least six atoms (e.g. Herbst & van Dishoeck, 2009, ARA&A).
complex organic molecule (COM)
molekul-e orgânik-e hamtâft
Fr.: molécule organique complexe
dense molecular cloud
abr-e molekuli-ye cagâl
Fr.: nuage moléculaire dense
A type of → interstellar medium cloud in which → carbon (C) becomes almost completely molecular due to relatively high → extinction. The chemistry is qualitatively different from that of → diffuse molecular clouds, as the → electron abundance is very low (→ cosmic-ray ionization being the dominant source) and the reactive C is replaced by the very stable → carbon monoxide (CO). This regime is found only in → sightlines with AV > 5-10 mag; not all such sightlines will contain dense cloud material and if dense cloud material is present it is likely to be surrounded by → translucent material. These clouds are typically → self-gravitating, and are most often observed by → infrared absorption and → millimeter wave emission methods. Their densities are typically at least 104 cm-3, and their → kinetic temperatures are typically on the order of 10-50 K in the quiescent regions. Most of the more than 140 currently known → interstellar molecules were found through observations of → microwave→ rotational transitions in such clouds, starting with the discovery of OH, followed by a host of other new detections such as CO, NH3, H2O, and H2CO (Snow & McCall, 2006, ARA&A 44, 367).
diffuse molecular cloud
abr-e molekuli-ye paxšidé
Fr.: nuage moléculaire diffus
A type of → molecular cloud in which the → interstellar radiation field is sufficiently attenuated, so that the local fraction of → molecular hydrogen (H2) becomes substantial (> 0.1). However, enough interstellar radiation is still present to → photoionize any atomic carbon, or to → photodissociate → carbon monoxide (CO) such that carbon is predominantly still in the form of C+ (> 0.5). In steady state, diffuse molecular clouds must necessarily be surrounded by diffuse atomic gas, in order to provide the → shielding of radiation. This means that most sightlines that cross a diffuse molecular cloud will also cross → diffuse atomic gas (Snow & McCall, 2006, ARA&A 44, 367).
giant molecular cloud (GMC)
abr-e molekuli-ye qulpeykar (#)
Fr.: nuage moléculaire géant
A massive complex of → interstellar gas and → dust, consisting mostly of → molecular hydrogen, that typically stretches over 150 light-years and contains several hundred thousand → solar masses. Giant molecular clouds are the principal sites of star formation. → molecular cloud.
Fr.: molécule homonucléaire
hot molecular core (HMC)
maqze-ye molekuli-ye dâq
Fr.: cœur moléculaire chaud
A relatively small, dense, and hot → molecular clump occurring in regions of → massive star formation. HMCs have diameters ≤ 0.1 pc, densities ≥ 107 cm-3, and temperatures ≥ 100 K. The densest hot cores are traced in → ammonia (NH3) and possess densities of 108 cm-3, sizes down to 0.05 pc and temperatures of up to 250 K. Hot molecular cores are generally associated with → compact H II regions and → ultracompact H II regions. High angular resolution observations suggest that HMCs are internally heated by embedded sources, since temperature and density increases toward the center as expected if star formation is occurring close to the core center. Same as → hot core.
Fr.: force intermoléculaire
A Force acting between molecules.
Fr.: molécule interstellaire
Any molecule that occurs naturally in clouds of gas and dust in the interstellar medium. So far more than 140 species have been discovered, many of which nonexistent on Earth.
Within the molecule; occurring by a reaction between different parts of the same molecule.
Fr.: molécule ionique
A molecule that consists of the ions of the chemical elements that make up the molecule.
mean molecular weight
vazn-e molekuli-ye miyângin (#)
Fr.: poids moléculaire moyen
The total atomic or molecular weight divided by the total number of particles. For instance, the mean molecular weight of a plasma of pure ionized 4He would be 4 (the atomic mass number) divided by 3, the total number of particles (1 nucleus plus 2 electrons), i.e. 4/3.
mol, molekul-geram, atom-geram
The → SI unit of amount of → substance; symbol mol. One mole contains exactly 6.022 140 76 × 1023 elementary entities. This number is the fixed numerical value of the → Avogadro constant, NA, when expressed in the unit mol-1.
From Ger. Mole, short for Molekül, from Fr. → molecule.
Of or pertaining to or caused by molecules.
Molekuli, from molekul→ molecule + -i adj. suffix.
bând-e molekuli (#)
Fr.: bande moléculaire
abr-e molekuli (#)
Fr.: nuage moléculaire
A relatively dense, cold region of interstellar matter where the atoms are primarily bound together as molecules rather than free atoms or ionized particles. Molecular clouds represent the coldest and densest phase of the → interstellar medium. They consist primarily of → molecular hydrogen (H2), with temperatures in the range 10-100 K. Molecular hydrogen is not directly observable under most conditions in molecular clouds. Therefore, almost all current knowledge about the properties of molecular clouds has been deduced from observations of molecules such as → carbon monoxide (CO), which have strong emission lines mainly in the → millimeter portion of the → electromagnetic spectrum. So far 129 molecular species have been detected in molecular clouds, among which complex organic molecules. → Dust grains in molecular clouds play a crucial role in the formation of molecules. Molecular clouds are the principal sites where stars form. → giant molecular cloud; → Orion molecular cloud.