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The work-function can be calculated from the difference in the photon energy of He (I) (21.2 eV) and the energy difference ΔE between the secondary cutoff energy (E cutoff) and the Fermi edge (E F) as shown in Fig. 5a as varPhi =21.2-varDelta E (2).
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On the other hand, the difference in the photon energy dependence between NaCl and LiF may be used to assess the mean effective energy of the photon field.
The simplest way is, as demonstrated above, to determine it from the difference in the peak photon energy or the difference between fluorescence and phosphorescence onsets [15].
Under light intensity of 15 µmol photons m−2 s−1, the difference in the Fv value between the strains was the smallest.
As can be seen, the difference in photon numbers is conserved while the sum of photon numbers is larger than 1 (amplification) and increases with increasing RI steepness.
This is to account for the difference in photon arrival times as Chandra orbits the Earth and the Earth moves around the Sun.
Before beginning any timing analysis, also complete the Apply Barycenter Correction thread to correct for the difference in photon arrival times as the Earth and Chandra move around the Sun.
The difference in phase of photons can be measured with huge accuracy, but even this has a limit, known as the standard quantum limit.
This is possible using photonics, where it involves sending single photons through a random unitary network and drawing samples from the output in the photon number basis.
For example, an atom may change spontaneously from one state to another state with less energy, emitting the difference in energy as a photon with a frequency given by the Bohr relation.
From these forms then, we can say that in the low-photon-number regime ((|alpha |^{2}<500)), the difference in these detection schemes can be significant, but in the high photon number regime ((|alpha |^{2}>10^{5})), there is little difference between the various detection schemes.
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