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Optical and nonthermal radio emissions point at an important role of accelerated electrons in the primary energy release.
The observed micro-events are secondary phenomena, and do not represent the primary energy release, nor its total amount.
The most intense radio emissions are not due to electron beams, but are post-flare emissions apparently not directly related to the primary energy release and acceleration process.
Stellar coronal energy losses are predominantly diagnosed by X-ray, extreme-ultraviolet, and radio emissions but they all are secondary products of the actual primary energy release.
Radio bursts with fine structures in decimetric centimetric wave range are generally believed to manifest the primary energy release process during flare/CME events.
The present paper discusses evidence and diagnostics for the primary energy release and energy transport, focusing on i) the hypothesis that active stellar coronae are heated by a stochastic sequence of flares, and ii) that these flares involve chromospheric evaporation to increase the coronal temperature, its emission measure, and the electron density.
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"The sooner we make a concerted effort to curtail the burning of fossil fuels as our primary energy source and releasing the C02 to the air, the lower our risk and cost will be".
During extratropical transition, the cyclone begins to tilt back into the colder airmass with height, and the cyclone's primary energy source converts from the release of latent heat from condensation (from thunderstorms near the center) to baroclinic processes.
We explicitly assume that the volumetric rate of chemical energy release in such "primary" combustion chambers is controlled by the liquid fuel physical vaporization process (with negligible lags due to propellant droplet heat-up or vapor-phase ignition).
According to the BP Statistical Review of World Energy 2009, released in June, global primary energy consumption — including oil, natural gas, coal, nuclear, and hydro power — grew by 1.4percentt last year, the slowest rate since 2001.
Its primary objective is to investigate particle acceleration and energy release in solar flares through imaging spectroscopy of flare hard X-ray/gamma-ray continuum and gamma-ray lines emitted by energetic electrons and ions, respectively.
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CEO of Professional Science Editing for Scientists @ prosciediting.com