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We start by analyzing EELS within a semiclassical framework, where a swift electron propagating with velocity v loses a tiny part of its kinetic energy by performing work against the electric field E[ re(t)] produced by itself.
When phonon conduction is non-negligible, the coefficient α is smaller than 1 and ZT is smaller than ZT 0. The formalism of the previous section explicitly shows that the transport properties of an electron propagating through a wire are sensitive to the energy dependence of the transmission coefficient.
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The non-linear ultrafast response is based on a plasmonically enhanced, multiphoton absorption resulting in a field emission of ballistic hot electrons propagating across the nanoscale junctions.
Initially we calculated radiation from electrons propagating in a uniform parallel magnetic field to verify the technique.
For such gaps with a distance of 1.1 µm (Fig. 4c), we cannot measure any time-integrated Iemission of photoemitted electrons propagating across the gap within the given noise level (data not shown), most likely because of the insulating properties of the Al2O3 substrate.
From these simulations we obtained spectra which are consistent with those generated from electrons propagating in turbulent magnetic fields with red noise.
However, when electrons propagate ballistically across the nanojunctions, a unipolar displacement current can couple into the THz striplines by near-field interactions, despite the frequency and momentum mismatch17.
The photocurrent Iemission is unipolar, and its polarity is such that electrons propagate from the emitter to the collector with an amplitude of 360 fA.
The energetic electrons propagate farther into the plasma to much higher densities where Coulomb collisions become important.
As our transconductance results are consistent with the picture that electrons propagate elastically along the rows, in order to gain further understanding we performed single-probe STM experiment on a clean Ge 001 -c(4 × 2) surface area near a sinGe 001 -ctomic step-edge (Fig. 3a, with structural details in Supplementary Note 6).
Nonthermal electrons propagate along the coronal magnetic field thereby exciting dm- and m-wave radio burst emission after acceleration during reconnection or other energy release processes in heights of some Mm to ⩾700 Mm.
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