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Now that the first proton collisions have been successfully carried out, scientists will start to gradually increase the particle intensity of the proton beams.
The results show that our simulation can closely reproduce observational data for the temporal evolution of particle intensity.
The particle intensity distribution in the transverse direction is assumed to be Gaussian with a full width at half maximum (FWHM) in the range of 1 4 mm.
Particle intensity distribution in the transverse direction is a Gaussian and the beam can be focused to a spot size with σ = 0.1 mm–1.0 mm.
Our approach centers on the observation that these shocks are often preceded by identifiable signatures in the energetic particle intensity data.
Based on the shape of the oxygen spectrum during the decay phase following the peak in particle intensity, each SEP event was categorized as either exponential (7 events) or power law (29 events).
Similar(48)
Periods with comparable particle intensities at ACE and Ulysses occurred during the decay phase of large SEP events.
It is shown that low-energy particle intensities are discontinuous and sharply peaked at the shock, consistent with the observations.
Energetic particle intensities observed by ERNE instrument onboard SOHO spacecraft during the first two years of SOHO science mission have been analysed and compared to observations of IMP 8 satellite around two earlier sunspot minima.
During an eight month period around the latest sunspot minimum, which occurred in October 1996, energetic particle intensities stayed at a lower level than during any equivalent period around solar minima of July 1976 and June 1986.
We discuss the formation of these periods of nearly identical particle intensities (i.e., "reservoirs") in terms of both fresh injections of solar energetic particles and the formation of compressed magnetic field regions in the heliosphere beyond the Earth orbit (∼2 5 AU).
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