<< < -es -it -sc 201 951 abe abs abs aca acc acc aco act ada adh ado aer aft air Alf alg alk alp Alt alt amb ana And ang ani ann ant ant ant apo app app Apu arc arg Arn art ass ast ast ast atm ato att aur aut avo azi bac bal bar bar bat Bea Bel bet bia big bin bio Bir bla bla blo Blu bol Boo bou box bre Bri bro bur cal cal Can cap car Car cat cau cel cen cen cha Cha cha che Chi chr cir cir civ cla clo clo CMB coa coe coh col col col com com com com com com com com Com con con con con con con con con con con con con coo cor cor cor Cos cos cos cou cou cra cri cro cry cul cur cyc D l dar dat day dea dec dec dec def def deg Del Den dep der det deu dew dic dif dif dil dip dir dis dis dis dis dis diu dog Dop dou Dra Dsc dus dwa dyn Dys Ear ecc eco edg egg Ein Ela ele ele ele ele ell eme emp enc eng ent epi equ equ equ eru eth Eur eve exa exc exe exi exo exp ext ext ext fab fai Fan fea fem fer fie fil fir fir fla fli flu foc for for for fra fre fre fri fun fuz gal gal gal Gam gau Gau gen geo geo geo geo Gib glo gov gra gra gra gra gre gro Gui H-a hal Ham har Hay hea hei hel Hel her het hie hig hoa hom hor hot Hub Hug hur hyd hyd hyl hyp ice ide ima ima imp imp inc inc ind ine inf inf inf ing inn ins ins int int int int int int int int inv inv ion iro Isl iso iso Jab jet Jov Jup Kar Kep kil Kip Kra Lag Lam Lan Lar las law lea Leg Leo lev lig lim lin lin lin lit loc loc log Lor low lum lun lun Lym Mac mag mag mag mag mag mai Mal map mas mas mat Mau mea mea med Men mer Mes Met met mic mic Mie mil min Mir mix mod mol mom Moo mor mov mul mur n-b nan nat nea neg Ner neu new New NGC noc nom non non nor nor nuc nuc nul nut obj obl obs occ oct off old one ope opp opt opt orb ord org Ori osc oth ove Owl P-s Pal par par par par Pas pat pec pen per per per per per Pha pha pho pho pho phy pie pix Pla pla pla pla Pli Poi pol pol pol pol por pos pos pow pre pre pre pre pri pri pri pro pro pro pro pro pro pro pub pul pyc qua qua qua qua qui rad rad rad rad rad rad rai ran rar Ray rea Rea rec rec red red ref ref reg rel rel rel ren res res res res ret rev Ric rig rin roc roo rot rot rur S5- Sal sat sca sca Sch sci Scu sec sec sed sel sel sem seq set sha she sho sid sie sil sim sin sit sky slo sno sod sol sol sol sol son sou spa spa spe spe spe spe sph spi spo squ sta sta sta sta ste ste ste Sti sto str str sub sub sub sul sup sup sup sup sur sur syl syn sys tal Tay tel ten ter tex the the the the Tho thr tid tim Tit too Tor tra tra Tra tra Tra tri Tri tru tub tur two Typ ult ult unc uni uni uni upl ura uti val var vec vel ver Ver vie vir vis vis vol W-R war wav wav wea Wei wha wid win WN3 Wol wri xen yok zen zij > >>
clover šabdar (#) Fr.: trèfle Any of various plants of the genus Trifolium with three round, green leaves that are joined together. Clovers occasionally have leaves with four leaflets, instead of the usual three. M.E. clovere; O.E. clafre; cf. M.L.G. klever, M.Du. claver, Du. klaver, O.S. kle, O.H.G. kleo, Ger. Klee "clover," of uncertain origin. Šabdar, of unknown origin. |
cloverleaf quasar (H1413+117) kuâsâr-e barg-e šabdar Fr.: quasar du trèfle à quatre feuilles A bright → quasar whose image is split into four spots due to → gravitational lensing (Magain et al. 1988, Nature 334, 325). The four images of comparable brightness all lie within 0.7 arc seconds of the image center. The quasar has a → redshift of 2.56, corresponding to a distance of about 11 billion → light-years. Observations indicate that the lensing galaxy is located approximately at the geometrical center of the four images. A firm spectroscopic redshift of the lens has yet to be obtained; however, a → cluster of galaxies at a redshift of z = 1.7 has been suggested to account for the lensing of this system. H1413+117 was the first quasar to be detected in the → submillimeter wave → continuum and in → carbon monoxide emission. So named because of the optical image; → clover; → leaf; → quasar. |
clump gude Fr.: grumeau 1) A compact mass, in particular that contained in a less dense environment. 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." |
clumped wind bâd-e gudedâr 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. |
clumpiness gudegi Fr.: grumelosité Of a → molecular cloud, the property of being
made up of → clumps. Clumpiness, from → clumpy + → -ness. Gudegi from gudé, → clump, + -gi suffix forming noun from adjectives ending in -é. |
clumping gudedâri Fr.: grumelage The massing together of material to form clumps. → wind clumping. |
clumping factor karvand-e gudedâri Fr.: facteur de grumelage The ratio fcl = <ρ2> / <ρ >2, where ρ represents the → stellar wind density and the brackets mean values. Unclumped wind has fcl = 1 and → clumping becomes significant for fcl≅ 4. |
clumpy gudedâr Fr.: grumeleux Of a → molecular cloud, being composed of → clumps. Clumpy, from → clump + -y suffix meaning "full of or characterized by," from O.E. -ig, from P.Gmc. *-iga, akin to Gk. -ikos, L. -icus, → -ics. 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." |
clumpy galaxy kahkešân-e gudedâr 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. |
cluster 1) xušé (#); 2) xušé bastan (#) Fr.: 1) amas; 2) s'agglomérer, se grouper 1) A group of the same astronomical objects gathered or occurring closely
together, such as → cluster of galaxies,
→ globular cluster, → open cluster,
and so on. O.E. clyster "cluster," probably akin to O.E. clott "clot". Xušé "cluster, a bunch of grapes, an ear of corn," (Laki huša), from Mid.Pers. hošag or xušak; cf. Skt. guccha- "bundle, bunch of flowers, cluster of blossom, clump;" xušé bastan, with bastan "to bind, shut; to clot; to form seed buds", from Mid.Pers. bastan/vastan "to bind, shut," Av./O.Pers. band- "to bind, fetter," banda- "band, tie," Skt. bandh- "to bind, tie, fasten," PIE *bhendh- "to bind," cf. Ger. binden, E. bind. |
cluster core maqze-ye xušé Fr.: cœur d'amas The central part of a cluster (globular, galaxies, etc.) where the spatial density of the objects making up the cluster is much higher than the average value. |
cluster formation efficiency (CFE) kârâyiè-ye diseš-e xuše Fr.: efficacité de formation d'amas The fraction of → star formation which happens in → bound clusters. It is defined as the ratio between the → cluster formation rate and → star formation rate (Bastian, 2008, MNRAS 390, 759, arxiv/0807.4687). → cluster; → formation; → efficiency. |
cluster formation rate (CFR) nerx-e diseš-e xuše Fr.: taux de formation d'amas A parameter used in star formation models representing the ratio of the total mass in → star clusters to the corresponding age range (Bastian, 2008, MNRAS 390, 759, arxiv/0807.4687). |
cluster mass function (CMF) karyâ-ye jerm-e xušé Fr.: fonction de masse d'amas An empirical power-law relation representing the number of clusters as a function of their mass. It is defined as: N(M)dM ∝ M -αdM, where the exponent α has an estimated value of about 2 and dM is the mass interval. It is believed that this is a universal law applying to a variety of objects including globular clusters, massive young clusters, and H II regions. |
cluster of galaxies xuše-ye kahkašâni (#) Fr.: amas de galaxies Same as → galaxy cluster. |
clustering xušé bandi Fr.: agglomération, groupement Grouping of a number of similar astronomical objects. Noun from verb → cluster. |
clustering law qânun-e xušé bandi Fr.: loi de groupement An empirical power-law representing the number of stellar clusters as a function of the number of stars per cluster within an interval. It is expressed as: N(N*) dN*∝ N*-α dN*, where N(N*) is the number of clusters containing N* stars and dN* is the interval in star number. It is believed that this relationship applies to a variety of systems, including stellar clusters, globular clusters, H II regions (Oey et al. 2004, AJ 127, 1632). → clustering; → law. |
clutter âluzé Fr.: A disorderly heap or assemblage; a state or condition of confusion. Variant of clotter (now obsolete), from to clot + -er. Âluzé, from Kurd. âluz, Tabari âluz, âliz "messy, disorderly, untidy," Dehxodâ âlofté "astonished; mad; broken," âloftan "to rage, grow mad." |
CMB CMB Fr.: CMB See → cosmic microwave background radiation (CMBR). CMB, short for → Cosmic → Microwave → Background. |
CMB angular power spectrum binâb-e tavâni-ye zâviye-yi-e CMB Fr.: spectre de puissance angulaire du CMB A plot displaying the amplitude of → cosmic microwave background anisotropy as a function of angular size or → multipole index. Same as → angular fluctuation spectrum. The plot, based the on WMAP and other data, shows a plateau at large angular or length scales (→ Sachs-Wolfe plateau), then a series of peaks at progressively smaller scales. These features arise from the gravity-driven acoustic oscillations of the coupled photon-baryon fluid in the early Universe (→ baryon acoustic oscillation). In particular, a strong peak is seen on an angular scale (at l ~220), corresponding to the physical length of the → sound horizon at the → recombination era. It depends on the curvature of space. If space is positively curved, then this sound horizon scale will appear larger on the sky than in a flat Universe (the first peak will move to the left). The second peak (l ~ 550), which is the first harmonic of the main peak, relates to the baryon/photon ratio. The third peak can be used to help constrain the total matter density. → angular; → fluctuation; → spectrum. |
<< < -es -it -sc 201 951 abe abs abs aca acc acc aco act ada adh ado aer aft air Alf alg alk alp Alt alt amb ana And ang ani ann ant ant ant apo app app Apu arc arg Arn art ass ast ast ast atm ato att aur aut avo azi bac bal bar bar bat Bea Bel bet bia big bin bio Bir bla bla blo Blu bol Boo bou box bre Bri bro bur cal cal Can cap car Car cat cau cel cen cen cha Cha cha che Chi chr cir cir civ cla clo clo CMB coa coe coh col col col com com com com com com com com Com con con con con con con con con con con con con coo cor cor cor Cos cos cos cou cou cra cri cro cry cul cur cyc D l dar dat day dea dec dec dec def def deg Del Den dep der det deu dew dic dif dif dil dip dir dis dis dis dis dis diu dog Dop dou Dra Dsc dus dwa dyn Dys Ear ecc eco edg egg Ein Ela ele ele ele ele ell eme emp enc eng ent epi equ equ equ eru eth Eur eve exa exc exe exi exo exp ext ext ext fab fai Fan fea fem fer fie fil fir fir fla fli flu foc for for for fra fre fre fri fun fuz gal gal gal Gam gau Gau gen geo geo geo geo Gib glo gov gra gra gra gra gre gro Gui H-a hal Ham har Hay hea hei hel Hel her het hie hig hoa hom hor hot Hub Hug hur hyd hyd hyl hyp ice ide ima ima imp imp inc inc ind ine inf inf inf ing inn ins ins int int int int int int int int inv inv ion iro Isl iso iso Jab jet Jov Jup Kar Kep kil Kip Kra Lag Lam Lan Lar las law lea Leg Leo lev lig lim lin lin lin lit loc loc log Lor low lum lun lun Lym Mac mag mag mag mag mag mai Mal map mas mas mat Mau mea mea med Men mer Mes Met met mic mic Mie mil min Mir mix mod mol mom Moo mor mov mul mur n-b nan nat nea neg Ner neu new New NGC noc nom non non nor nor nuc nuc nul nut obj obl obs occ oct off old one ope opp opt opt orb ord org Ori osc oth ove Owl P-s Pal par par par par Pas pat pec pen per per per per per Pha pha pho pho pho phy pie pix Pla pla pla pla Pli Poi pol pol pol pol por pos pos pow pre pre pre pre pri pri pri pro pro pro pro pro pro pro pub pul pyc qua qua qua qua qui rad rad rad rad rad rad rai ran rar Ray rea Rea rec rec red red ref ref reg rel rel rel ren res res res res ret rev Ric rig rin roc roo rot rot rur S5- Sal sat sca sca Sch sci Scu sec sec sed sel sel sem seq set sha she sho sid sie sil sim sin sit sky slo sno sod sol sol sol sol son sou spa spa spe spe spe spe sph spi spo squ sta sta sta sta ste ste ste Sti sto str str sub sub sub sul sup sup sup sup sur sur syl syn sys tal Tay tel ten ter tex the the the the Tho thr tid tim Tit too Tor tra tra Tra tra Tra tri Tri tru tub tur two Typ ult ult unc uni uni uni upl ura uti val var vec vel ver Ver vie vir vis vis vol W-R war wav wav wea Wei wha wid win WN3 Wol wri xen yok zen zij > >>