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- W2006014767 abstract "The concept of the nanoflare, used in interpreting the solar X-ray corona, is extended to RS CVn stars which, unlike the Sun, exhibit non-thermal quiescent radio spectra. The theoretical synchrotron-radiation radio spectrum emitted by a regular series of nanoflare-electron pulses, injected into the coronal magnetic field, is derived: for an electron energy spectrum N(γ)∝γ−s, the spectral power density is given by P(ν)∝ν−s/2. This result is valid for the observation of a series of nanoflares with total time duration ≳ the characteristic electron radiation lifetime, which is the case for electrons trapped in extensive coronal regions such as exist in RS CVn stars on the magnetic-dipole magnetospheric model. The tenuous coronal plasma allows the electrons to give a radio spectrum unaffected at high frequencies (≳5 GHz) by electron collision loss, while the emission of bremsstrahlung X-rays by the electrons also occurs with a spectrum that is related to their radio emission. The observation of individual X-ray bursts, which would provide direct evidence for microflares, is not, however, attainable with current instrumentation." @default.
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- W2006014767 date "1999-12-11" @default.
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- W2006014767 title "The nanoflare model and stellar quiescent radio emission" @default.
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- W2006014767 doi "https://doi.org/10.1046/j.1365-8711.1999.02979.x" @default.
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