mâseš-e qobâr, roceš-e ~
Fr.: coagulation de la poussière
Fr.: tourbillon de poussière
A small but vigorous → whirlwind, usually of short duration, rendered visible by → dust, → sand, and → debris picked up from the ground (Meteorology Glossary, Amer. Meteo. Soc.). See also → dust storm, → dust whirl.
Fr.: émission des poussières
Thermal emission in infrared from interstellar → dust grains receiving photons. Dust grains absorb ultraviolet and visible light emitted by nearby stars and re-radiate in the infrared wavelengths. Since the infrared light is of lower energy than the ultraviolet/visible light, the difference goes into heating the dust grain. Typical temperatures for interstellar grains are tens of degrees Kelvin.
Fr.: marque de poussière, signature de ~, motif spectral de ~
An emission or absorption mark in the spectrum of an astronomical object, the origin of which is attributed to the presence of dust in the object or on the line of sight.
dâne-ye qobâr (#)
Fr.: grains de poussière
A small, solid flake of → graphite and/or → silicates coated with water ice, found in the → interstellar medium or the → interplanetary medium. Dust grains are irregularly shaped with sizes from microns to Angstroms (→ very small grain; → big grain; → PAH). It is believed that the dust is mainly formed in the cool outer layers of → red giants and dispersed in the interstellar medium. In dense environments, such as → molecular clouds and around → protostars, dust grains grow due to collisions (→ grain growth). Therefore, dust grains in → protostellar disks should be larger than interstellar grains. Dust grains absorb and scatter optical and ultraviolet light and re-radiate in infrared (→ dust emission). Dust acts as a catalyst in the interstellar medium, because molecules form via reactions on the surface of dust grains.
Fr.: bande de poussière
A narrow, elongated structure of absorbing matter seen running over extended emission objects such as nebulae and galaxies.
→ dust; lane, from O.E. lane, lanu "narrow hedged-in road," cf. Du. laan "lane," O.N. lön "row of houses," of unknown origin.
Bâriké "a narrow thing," from bârik "narrow," from Mid.Pers. bārīk "narrow," Av. bāra-, as in tiži.bāra- "sharp-edged," from brāy- "to cut," Mod.Pers. bor-, boridan "to cut;" qobâr→ dust.
Fr.: modèle de poussière
A model of → dust grains conceived to describe the observed → interstellar extinction properties. It is characterized by the abundance of the different → chemical elements locked up in the dust, and by the → composition, → morphology, and → size distribution of its individual grains. For example, → MRN dust model.
tirešod pat qobâr
Fr.: obscurcissement par la poussière
parâkaneš-e qobâri, ~ pat qobâr
Fr.: diffusion par la poussière
Fr.: dépose de poussières
A process occurring in → protoplanetary disks whereby relatively large → dust grains settle to the disk midplane. These grains, with sizes from → micron to → millimeter, grow from smaller dust grains and will eventually give rise to a planetary system.
Fr.: tempête de poussière
donbâle-ye qobâri (#)
Fr.: queue de poussière
Fr.: température de poussière
An indication of the heat amount received by → dust grains from the ambient → radiation field. Dust temperature depends on the optical properties and → sizes of grains (i.e., on the way they → absorb and → emit radiation) as well as on the → interstellar radiation field. Most of the visible and → ultraviolet radiation in galaxies from stars passes through clouds of particles and heats them. This heating leads to re-radiation at much longer wavelengths extending to the millimeter.
Fr.: tourbillon de poussière
A rapidly rotating column of air (whirlwind) over a dry and dusty or shady area, carrying dust, leaves, and other light material picked up from the ground (Meteorology Glossary, Amer. Meteo. Soc.). See also → dust devil, → dust storm.
Fr.: vent induit par poussière
A → stellar wind generated by the action of → radiation pressure on dust grains. This occurs in the case of cool stars, such as → AGB stars, with → effective temperatures below 2500 K when the density is sufficiently large. Since dust is a very good continuum absorber, the dust grains will be radiatively accelerated outward.
1) Something that one is expected or required to do by moral or legal
M.E. du(e)te, from Anglo-Fr. duete, from O.Fr. deu "due, owed; proper, just," from V.L. *debutus, from L. debitus, p.p. of debere "to owe."
Harg, from Mid.Pers. harg, halg "duty, tribute; work, effort;" akin to Mod.Pers. gahulidan "to exchange, barter," → exchange; cf. Wakhi (y)ark "work, matter, business", Yaghnobi ark "work, matter, business," Yighda hor, Munji hôr(g) "work;" Proto-Ir. *harH- "to pay tribute; to barter, trade, exchange;" cognate with Gk. elein "to take (by force)," elor "loot, looty, catch;" E. to sell (Cheung 2006).
1) General: A person of abnormally small height owing to a pathological
condition; an animal or plant much smaller than the average of its kind or
Dwarf, from ME dwerg, dwerf, O.E. dweorg, dweorh, O.H.G. twerg "dwarf," from P.Gmc. *dweraz.
Kutulé, from kut "small, short" + Pers. diminutive suffix -ulé, → -ula. The first component kut is the base of kutâh "short, small, little," kudak "child, infant," Mid.Pers. kôtâh "low," kôtak "small, young; baby;" the Mid/Mod.Pers. kucak "small," belongs to this fammily; Av. kutaka- "little, small."
Fr.: céphéide naine
An old name for a class of pulsating variable stars with small variations in amplitude, also called an AI Velae star or delta Scuti star. They lie in the lower part of the Cepheid instability strip.
dwarf elliptical galaxy
kahkašân-e beyzigun-e kutulé (#)
Fr.: galaxie elliptique naine
A galaxy that is much smaller than other members of the elliptical class; it is designated as dE. A subtype of dwarf ellipticals is called a → dwarf spheroidal galaxy (dSph). The basic characteristics of the class are low surface brightness and smooth light distribution. They range in luminosity from that of the faintest dSph galaies MV ~ -9 to about -17. In the → Local Group there are 19 known dEs. They are very common in → galaxy clusters.
kahkešân-e kutulé (#)
Fr.: galaxie naine
A small, low luminosity galaxy that is associated with a larger spiral galaxy and may make up part of a galactic halo. There are many of them in the Local Group, and often orbit around larger galaxies such as the Milky Way and the Andromeda Galaxy. There are three main types of them: → dwarf elliptical galaxy (dE), → dwarf irregular galaxy (dI), and → dwarf spiral galaxy (dSA).