Fr.: non lié
Fr.: charge non liée
Same as → free charge.
Fr.: amas non lié
A cluster of objects, such as stars or galaxies, in which the members are not tied together gravitationally. In such a cluster the members scatter through space following different directions. → bound cluster.
Fr.: système non lié
An association of bodies which are not gravitationally tied together.
unbound young stellar system (UYSS)
râžmân-e setâre-yi-ye javân-e nâbandidé
Fr.: système stellaire jeune non lié
A class of gravitationally loose stellar conglomerate with a notable apparent shape making it different from typical → bound → star clusters. The UYSS class includes a large range of objects, which extend at various size scales and at various degrees of self-binding; from small (semi-)compact → unbound systems named → stellar associations, to huge extended superstructures of → massive stars that make up whole parts of Galactic → spiral arms, known as → stellar complexes (Gouliermis, D. A., 2018, PASP 130:072001; arXiv:1806.11541).
Fr.: fonction non bornée
The function y = f(x) in a given range of the argument x if there is no number M such that for all values of x in the range under consideration the inequality | f(x) | ≤ M will be fulfilled. → bounded function.
The state of being uncertain; unpredictability; indeterminacy. → uncertainty principle.
Fr.: principe d'incertitude
A quantum mechanical principle due to Werner Heisenberg which states that the position and momentum of a particle cannot be determined simultaneously with any arbitrary accuracy. These quantities can be determined only with accuracies limited by the relation Δx.Δp ≥ (1/2)ħ, where Δx is the error in the determination of the position and Δp is the error in the momentum. A similar relation holds for the energy of a particle and the time, ΔE.Δt ≥ (1/2)ħ. Same as → Heisenberg uncertainty principle.
unclassified B[e] star (unclB[e])
setâre-ye B[e]-ye bi radé
Fr.: étoile B[e] non-classée
A temporary designation for a → B[e] star that cannot be placed in any of the four known classes.
Fr.: non clair
Difficult to see, hear, understand, or to be sure about.
Not limited by conditions; absolute.
Fr.: non conscient
Not awake and aware; not responding to one's environment.
Fr.: non conscience
A dune on a planetary surface, used in plural form undae.
From L. unda "wave," cognate with → water.
Šen-tal, from šen "sand" + tal "hill, heap."
Fr.: sous-, faible
A prefixal use of under, as to indicate place or situation below or beneath. Contrary to → over-.
M.E., from O.E. (cf. O.H.G. untar, Ger. unter, Goth. undar), from PIE *ndhero- "lower;" cf. Av. aδara- (adj.), aδairi- (prep.) "below;" Mid.Pers. êr "below, down; low, under," adar "low," azêr "below, under" (Mod.Pers. zir "below, down"); Skt. ádhara- "lower;" O.E. under "under, among").
Kam- "little, few; deficient, wanting; scarce" (Mid.Pers. kam "little, small, few," O.Pers./Av. kamna- "small, few").
The abundance of a chemical element being lower than a reference value, in particular compared to that of the Sun.
Fr.: amortissement faible
The behavior of a damped system when the amount of damping is weak so that the system oscillates with the amplitude gradually decreasing to zero. → overdamping.
1) kam-baravardan; 2) kam-baravard
Fr.: 1) sous-estimer; 2) sous-estimation
1) To estimate at too low a value, rate, or the like.
Insufficiently qualified for a particular job (OxfordDictionaries.com).
The circumstance in which there are not enough pixels in a star's image. The number of pixels that make up a star's image is determined by the relationship between the telescope focal length, the physical size of the pixels, and the size of the star's image. With an undersampled image it is not possible to obtain accurate estimates of the star's image size or its position. Undersampling occurs when the atmospheric seeing conditions are exceptionally good and the pixel size not small enough.