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With the flux distribution of each line, we conclude that the diffuse X-ray plasma exhibits lower temperature at larger Galactic latitude than that at smaller latitude.
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The proposed profile of the resonant region can interpret also the results obtained at other cusp/auroral stations and appears consistent with that one inferred in the northern hemisphere at smaller latitudes.
Typical ε values at low latitude are smaller than 4 m/s, as shown below.
As discussed earlier, Friedman et al. (2003) reports that the nocturnal temperature variation at a given altitude in the MLT region is small over the low latitude site, Arecibo Observatory (latitude: 18.6° N).
In the spectra taken near lunar poles, the instrument showed prominent absorption bands at 2.8-3 micorrespondingonding to OH/H2O but these bands were negligibly small in the low latitude spectra [26].
The values obtained for (varepsilon_{u}) and (varepsilon_{v}) are rather small at low latitudes, which indicate good precision; stipples in Fig. 7 show where their values are smaller than 4 m/s.
Because the Sun, with respect to Earth, migrates annually between the Tropic of Cancer and the Tropic of Capricorn, the yearly change in heating of Earth's surface is small at low latitudes and large at mid- and higher latitudes.
We also estimated the magnetic field variation due to prompt penetration electric fields, which is found to be very small at low latitudes in the present case.
The Sino-Magnetic Array at Low Latitudes (SMALL) is an ongoing project for the development of a two-dimensional (2-D) ground-based magnetometer array in China.
This UCLA-built instrument was originally designed for the Sino-Magnetic Array at Low Latitudes (SMALL) survey, a project to build a modern magnetometer array across China (Gao et al., 2000).
The most significant variation was the annual component with smaller amplitudes at low latitudes and larger amplitudes at higher latitudes.
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