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词汇 example_english_binding-energy
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Examples of binding energy


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These atoms will immediately leave the solid if their energy instantaneously increases in excess of the bindingenergy.
This is plausible because only a few collisions can lead to some atoms gaining enough energy to exceed the bindingenergy.
The core state bindingenergy in metal is therefore measured relative to the bottom of the conductivity band.
Any elastic or other deformations accompanying adhesion tend to increase the bindingenergy significantly and, to a lesser extent, the adhesion force.
Because of the strong dependence of the bindingenergy on local geometry and chemistry, the bond energy falls off rapidly with distance.
The different, labeled amino acids in the figure all contribute to the total biotin bindingenergy.
The difference in mass, 0.0011, then represents the bindingenergy of the two particles and corresponds to 1 million electron volts.
This preferred handedness is remarkable because the difference in bindingenergy between righthanded and left-handed (levorotatory) sugars is extremely tiny (relative energy difference : 10x17).
Both of these changes likely contribute to the loss in enthalpic bindingenergy observed for this compound.
In pairwise additive-force models the barrier from entropy loss nearly uniformly compensates for bindingenergy : these terms are very finely balanced.
The diffusing molecules differ greatly in size, spatial structure, polarity, bindingenergy, escape time and other properties affecting their progress through hydrophilic and hydrophobic regions of the cell.
Thirdly, we need a new generation of bindingenergy interdependence clauses.
From Europarl Parallel Corpus - English
You do not even dare to discuss a bindingenergy efficiency target.
From Europarl Parallel Corpus - English
Ensure that we have bindingenergy efficiency targets that are actually complied with.
From Europarl Parallel Corpus - English
The bindingenergy varies with the combination of the adsorbate and surface.
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Nickel-62 has the highest bindingenergy per nucleon of any isotope for any element, when including the electron shell in the calculation.
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The singlet deuteron is a virtual state, with a negative bindingenergy of.
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Every satellite has its own orbit, and practically any orbital distance, and any satellite bindingenergy, is possible.
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An electron is normally found in the lowest energy level, with the largest bindingenergy.
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Results from the calculations can include the bindingenergy.
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In inelastic collisions, kinetic energy is dissipated in various forms of energy, such as heat, sound, bindingenergy (breaking bound structures).
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The energy necessary to remove an electron from its shell (taking it to infinity) is called the bindingenergy.
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For every element and core (atomic orbital) there will be a different bindingenergy.
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In silico calculations show that 75% of the bindingenergy is derived from the forward donation and 25% from backdonation.
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The acceptor material needs a suitable energy offset to the bindingenergy of the exciton to the absorber.
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However, to quantify cooperativity in a hostguest system, the bindingenergy needs to be considered.
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The most massive stars that exist today may be completely destroyed by a supernova with an energy greatly exceeding its gravitational bindingenergy.
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In other words, at this extremely high temperature, the photons' kinetic energy would overwhelm the bindingenergy of the strong nuclear force.
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In other words, most of what composes the mass of ordinary matter is due to the bindingenergy of quarks within protons and neutrons.
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In this particular example, the electron bindingenergy has the same magnitude as the electron affinity for the neutral chlorine atom.
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Fe is greater than the nucleon-specific bindingenergy of very heavy nuclei, so that energy is released when heavy nuclei are broken apart.
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This helium-4 bindingenergy also accounts for why it is a product of both nuclear fusion and radioactive decay.
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This is due to the very high nuclear bindingenergy (per nucleon) of helium-4 with respect to the next three elements after helium.
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Using the liquid drop model for atomic nuclei, one can derive a semiempirical formula for the bindingenergy of a nucleus.
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This definition corresponds to a "positive" bindingenergy.
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The bindingenergy of nuclei is usually a positive number, since most nuclei require net energy to separate them into individual protons and neutrons.
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This calculation gives the loop energy of the order of bindingenergy.
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The kinetic energy of the emitted electron is equal to the transition energy in the nucleus, minus the bindingenergy of the electron.
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With more thermal energy released than the star's gravitational bindingenergy, it is completely disrupted; no black hole or other remnant is left behind.
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In metals, the electrons with no bindingenergy are called free electrons.
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In such cases, the bindingenergy is observed as a mass defect or deficit in the new system.
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These give predictions for the bindingenergy and lifetime of the states.
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The missing rest mass must therefore reappear as kinetic energy released in the reaction; its source is the nuclear bindingenergy.
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This is the region of nucleosynthesis within which the isotopes with the highest bindingenergy per nucleon are created.
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In contrast, if less than half of the valence band is filled, the band center is higher than bulk, and the bindingenergy decreases.
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When the x-ray energy corresponds to the bindingenergy of a core-level electron, this scattering process is resonantly enhanced by many orders of magnitude.
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This notable difference is a measure of the nuclear bindingenergy, which is a result of forces that hold the nucleus together.
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Over their lifetimes, protostars radiate a total energy comparable to their bindingenergy.
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The energy of the photons from positronium should differ slightly by the bindingenergy of the molecule.
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It is possible that the nuclei at the surface are iron, due to iron's high bindingenergy per nucleon.
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For nuclei heavier than nickel-62 the bindingenergy per nucleon decreases with the mass number.
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At the nuclear level, bindingenergy is also equal to the energy liberated when a nucleus is created from other nucleons or nuclei.
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Its mass fraction gravitational bindingenergy would then be 0.187, 18.7% (exothermic).
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These nuclides are local maxima in terms of bindingenergy for a given mass number.
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The other is the release of excess gravitational bindingenergy.
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The electric repulsion between each pair of protons in a nucleus contributes toward decreasing its bindingenergy.
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A bindingenergy suggests two or more particles or other entities that are bound together in the superconducting state.
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This high incidence is related to the stability (high bindingenergy) of the alpha particle, which makes more energy available to the reaction.
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Solids in general have a crystalline structure instead of an amorphous structure because the crystalline structure has a stronger bindingenergy.
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In a stable orbit the bindingenergy is a local minimum relative to parameter perturbation.
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The energy comes from the gravitational bindingenergy of a neutron star.
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The atom can be ionized if a collision with another particle supplies at least this bindingenergy.
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The bindingenergy per nucleon increases with mass number up until nickel-62.
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If this bindingenergy were retained in the system as heat, its mass would not decrease.
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This lost energy, necessary to overcome the potential barrier in order to separate the objects, is the bindingenergy.
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However, bindingenergy lost from the system (as heat radiation) would itself have mass, and directly represents the mass deficit of the cold, bound system.
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In astrophysics, gravitational bindingenergy of a celestial body is the energy required to expand the material to infinity.
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The biexciton bindingenergy in semiconductor quantum dots has been the subject of extensive theoretical study.
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Thus, a biexciton bindingenergy exceeding the inhomogeneous exciton line width is predicted for a wide range of nanotubes.
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Conversely, energy is released when a nucleus is created from free nucleons or other nuclei: the nuclear bindingenergy.
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The physical basis for this phenomenon also comes from the pairing effect in nuclear bindingenergy, but this time from both protonproton and neutronneutron pairing.
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The energy of a nucleon in a nucleus is its rest mass energy minus a bindingenergy.
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This study illustrates that entropy rather than enthalpy determines the bindingenergy of the system leading to negative cooperativity.
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An exception to this general trend is the helium-4 nucleus, whose bindingenergy is higher than that of lithium, the next heaviest element.
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It also helps to predict the nuclear bindingenergy.
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In the event the electron absorbs a quantity of energy less than the bindingenergy, it will transition to an excited state.
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In order for fission to produce energy, the total bindingenergy of the resulting elements must be less negative (higher energy) than that of the starting element.
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If new bindingenergy is available when light nuclei fuse, or when heavy nuclei split, either of these processes result in releases of the bindingenergy.
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When adding nucleons (protons or neutrons) to a nucleus, there are certain points where the binding energy of the next nucleon is significantly less than the last one.
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The transition energy can be coupled to a second outer shell electron, which will be emitted from the atom if the transferred energy is greater than the orbital bindingenergy.
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The larger the bindingenergy, the stronger the bond.
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Mathematical analysis of the theory delivers an equation which attempts to predict the bindingenergy of a nucleus in terms of the numbers of protons and neutrons it contains.
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For example, in the shell model, a proton and a neutron with overlapping wavefunctions will have a greater strong interaction between them and stronger bindingenergy.
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When such cascades recoil and reach the target surface with an energy greater than the surface bindingenergy, an atom would be ejected, known as sputtering.
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The greater the mass defect, the larger the bindingenergy.
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In nuclear reactions, however, the fraction of mass that may be removed as light or heat, i.e., bindingenergy, is often a much larger fraction of the system mass.
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The small bindingenergy makes the benzene dimer difficult to study experimentally, and the dimer itself is only stable at low temperatures and is prone to cluster.
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Helium-4 has an anomalously large bindingenergy because its nucleus consists of two protons and two neutrons; so all four of its nucleons can be in the ground state.
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This will alter the binding energies of the neighboring atoms and their coupling to crystal lattice.
A nucleon at the surface of a nucleus interacts with fewer other nucleons than one in the interior of the nucleus and hence its bindingenergy is less.
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Ubiquitousness and stability of atoms relies on their bindingenergy, which means that an atom has a lower energy than an unbound system of the nucleus and electrons.
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The difference in system masses, called a mass defect, is a measure of the bindingenergy in bound systems in other words, the energy needed to break the system apart.
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Many of these appear to be fairly uniform, so by the virial theorem, the total kinetic energy should be half the total gravitational bindingenergy of the galaxies.
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When the hydrogen fuel is exhausted, nuclear fusion can continue with progressively heavier elements, although the net energy released is lower because of the smaller difference in nuclear bindingenergy.
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These examples are from corpora and from sources on the web. Any opinions in the examples do not represent the opinion of the Cambridge Dictionary editors or of Cambridge University Press or its licensors.
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