Clump, from Du. klomp "lump, mass," or Low Ger. klump.
Gudé "ball, bowl, tumour" in Gilaki, cf. Skt. guda- "ball, mouthful, lump, tumour," Gk. gloutos "rump," L. glomus "ball," globus "globe," Ger. Kugel, E. clot, PIE *gel- "to make into a ball."
Fr.: vent grumelé
A → radiation-driven wind of → Wolf-Rayet and → O stars, which is not homogeneous, and contains compressions and rarefactions in the form of density clumps. Observationally, wind clumping appears as moving, small-scale structures in spectral line profiles. Indirect indicators of wind clumping include: electron scattering wings of emission lines, too-weak observed UV line profiles, and shapes of X-ray lines. The most likely physical explanation for the presence of these clumps is an instability in radiatively-driven winds. The inclusion of a clumping factor in the models of W-R winds reduces the → mass loss rates by a factor ~ 2-4 relative to homogeneous models. See also → clumping factor.
Gudegi from gudé, → clump, + -gi suffix forming noun from adjectives ending in -é.
The massing together of material to form clumps. → wind clumping.
Fr.: facteur de grumelage
Gudedâr, from gudé, → clump, + dâr "having, possessor," from dâštan "to have, to possess," O.Pers./Av. root dar- "to hold, keep back, maitain, keep in mind," Skt. dhr-, dharma- "law," Gk. thronos "elevated seat, throne," L. firmus "firm, stable," Lith. daryti "to make," PIE *dher- "to hold, support."
Fr.: galaxie grumeleuse
An irregularly shaped, clumpy → star-forming galaxy that does not fall anywhere on the → Hubble sequence and appears frequently at → redshifts z ~ 1-4. Galaxies at z ≤ 1 with similar morphologies and enhanced → star formation have been identified, but become less common with decreasing redshift. Clumpy galaxies are prominent in the → early Universe.
Fr.: milieu inter-grumeau
Fr.: grumeau moléculaire
One of many compact and dense sub-structures in a → molecular cloud. Their typical sizes are about 0.5-10 → parsecs and their masses range from about 50 to 103 → solar masses. The gas temperatures are about 10-20 K, and the number densities from about 103 to 104 cm-3.
Fr.: grumeau rouge
A concentration, on the → horizontal branch, of → red giant stars that roughly have the same intrinsic brightness. These core → helium burning stars are the metal rich equivalents of the better known → horizontal branch stars. Theoretical models predict that their absolute luminosity only weakly depends on their age and chemical composition.
red clump star
setâre-ye gude-ye sorx
Fr.: étoile du grumeau rouge
Fr.: grumelage de vent