Fr.: équivalence masse-énergie
The principle of interconversion of mass and energy, described by the → mass-energy relation.
Fr.: relation masse-énergie
The famous equation proposed by Einstein as a consequence of his special theory of relativity describing the equivalence of mass and energy: E = mc2, where E is energy, m is the equivalent amount of mass, and c is the velocity of light.
Fr.: énergie mécanique
1) taškidan; 2) taškândan
1) (v.intr.) To become combined, united, swallowed up, or absorbed; lose identity by
uniting or blending.
From L. mergere "to dip, immerse," probably rhotacized from *mezgo, and cognate with Skt. majj- "to dive, to sink," majjati "dives under;" Lith. mazgoju "to wash."
Taškidan, taškândan, from Gilaki tašk "tie, knot;" Tabari tešk "knot" + -idan infinitive suffix.
A hypothetical → transient event undergone by a → star due to its violent → merging with another star in a → close binary star. The release of → orbital energy causes the → envelope of the star to heat up and → inflate, causing the star to brighten considerably. Mergebursts are predicted to rival or exceed the brightest classical → novae in luminosity, but to be much cooler and redder than classical novae, and to become slowly hotter and bluer as they age.
1) tašké; 2) tašk
Fr.: fusion, coalescence
1) Any combination of two or more bodies into a single body. In particular, the formation
of a galaxy from the collision of two or more separate galaxies.
From → merge + -er (as in waiver).
Tašké; tašk, nouns from taškidan, → merge.
Fr.: processus de fusion
The process of collision between galaxies which leads to a single galaxy.
Fr.: arbre de coalescence
A method used in → numerical simulations for studying the growth and development of galaxies and → dark matter halos. Within the currently accepted ΛCDM cosmology, dark matter halos merge from small → clumps to ever larger structures. This merging history can be traced in simulations and stored in the form of merger trees. Merger trees are necessary because a galaxy may have more than one → progenitor at an early time.
Fr.: 1) fusion
1) (n.) The act of joining together as one, such as galaxy
Noun from → merge.
Fr.: galaxies en coalescence
Two or more galaxies that collide and merge into one galaxy.
Fr.: fusion mineure
The → merging in which one of the galaxies is significantly larger than the other (mass ratios above 10). The larger galaxy will often "swallow" the smaller satellite galaxy. The swallowed galaxy can trigger disk and nuclear star formation or activate a central core with shells that surround the predator.
Fr.: fusion mixte
Fr.: énergie nucléaire
Energy released during a nuclear reaction as the result of the conversion of mass into energy. → mass-energy equivalence.
Fr.: énergie orbitale
Fr.: énergie de parité
In nuclear physics, the extra binding energy associated with pairs of nucleons of the same kind. This quantity expresses the fact that nuclei with odd numbers of neutrons and protons have less energy and are less stable than those with even numbers of neutrons and protons.
periodically variable supergiant (PVSG)
abarqul-e vartande-ye dowreyi
Fr.: supergÃ©ante variable pÃ©riodiquement
A variable → supergiant star with typical periods of the order of 10 to 100 days and amplitudes less than a few tenths of a magnitude. PVSGs are thought to be pulsating → g modes, caused by a density inversion, arising from an → opacity bump, most likely from Fe, H, and/or He.
Fr.: énergie de Planck
The unit of energy in the system of Planck units. EP = √ (ħ c5/G) ≅ 1.22 x 1019 GeV. It can also be defined as EP = ħ / tP, where tP is the Planck time. This is an extraordinarily large amount of energy on the subatomic scale and particle accelerators have yet to produce a particle with this magnitude of energy. Understanding the properties of a subatomic particle that contains the Planck Energy is helpful in developing a Unified Field Theory which encompasses the realms of Quantum Theory and Relativity, although this too has evaded complete scientific understanding.
Fr.: énergie potentielle
Of a system, the work done in changing the system from some standard configuration to its present state. Thus, if a body of mass m is raised vertically through a height h, the work done, mgh, is the increase in potential energy.
potential energy curve
xam-e kâruž-e tavand
Fr.: courbe de l'energie potentielle
A plot that displays the → potential energy of a moving body as a function of its position. It is explained by the → conservation of energy and the conversion of potential energy into → kinetic energy and vice versa.
Fr.: énergie radiative