Resonant coronal acceleration on the Sun and in planetary nebulae

Details Resonant coronal acceleration on the Sun and in planetary nebulae Resonant coronal acceleration on the Sun and in planetary nebulae

Nov 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aps..dppfo1006r&link_type=abstract

American Physical Society, 44th Annual Meeting of the Division of Plasma , abstract #FO1.006

Astronomy and Astrophysics

Astrophysics

Scientific paper

Processes of ion energization in the weakly magnetized and dilute interplanetary medium or in the strongly magnetized and dense solar corona form a convenient prototype of laboratories for stellar and galactic plasma processes. While the heliospheric in-situ acceleration is due to propagating intreplanetary shocks, one of the most significant coronal acceleration processes include impulsive flares which were shown to correlate with the spectacular increase in the isotopic abundance ratio of He-3/He-4 by a factor of ˜1000 and the ratio Fe/O by a factor of ˜10. This selective energization of minority coronal ions in impulsive flares serves as an important tool to delineate relevant physical mechanisms which operate in the solar corona and affect the heliospheric nebula. The energization is due to a resonant interaction between a subset of coronal elements and isotopes with electromagnetic waves, which are excited during a major reconfiguration of magnetic field, either on the flaring coronal (deduced from the bremsstrahlung related electron fluxes) or on the active terrestrial auroral field lines (observed in situ as correlated to enhanced electron fluxes). Inclusion of these processes into the more intense long-duration acceleration by interplanetary shocks gives a new heliospheric baseline abundances of minority elements during active periods. It is suggested that a similar process may explain the enrichment. of minority elements in planetary nebulae, solving partly the "astrophysical ^3He problem", with important implications for the galactic evolution.

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