The nanoflare model and stellar quiescent radio emission

Details The nanoflare model and stellar quiescent radio emission The nanoflare model and stellar quiescent radio emission

Dec 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999mnras.310..784f&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 310, Issue 3, pp. 784-788.

Astronomy and Astrophysics

Astronomy

Radiation Mechanisms: Non-Thermal, Stars: Coronae, Stars: Individual: Ux Arietis, Stars: Magnetic Fields, Radio Continuum: Stars, X-Rays: Stars

Scientific paper

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 (>~5GHz) 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.

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