Filamentary structure on the Sun from the magnetic Rayleigh-Taylor instability

Details Filamentary structure on the Sun from the magnetic Rayleigh-Taylor instability Filamentary structure on the Sun from the magnetic Rayleigh-Taylor instability

Mar 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005natur.434..478i&link_type=abstract

Nature, Volume 434, Issue 7032, pp. 478-481 (2005).

Physics

61

Scientific paper

Magnetic flux emerges from the solar surface as dark filaments connecting small sunspots with opposite polarities. The regions around the dark filaments are often bright in X-rays and are associated with jets. This implies plasma heating and acceleration, which are important for coronal heating. Previous two-dimensional simulations of such regions showed that magnetic reconnection between the coronal magnetic field and the emerging flux produced X-ray jets and flares, but left unresolved the origin of filamentary structure and the intermittent nature of the heating. Here we report three-dimensional simulations of emerging flux showing that the filamentary structure arises spontaneously from the magnetic Rayleigh-Taylor instability, contrary to the previous view that the dark filaments are isolated bundles of magnetic field that rise from the photosphere carrying the dense gas. As a result of the magnetic Rayleigh-Taylor instability, thin current sheets are formed in the emerging flux, and magnetic reconnection occurs between emerging flux and the pre-existing coronal field in a spatially intermittent way. This explains naturally the intermittent nature of coronal heating and the patchy brightenings in solar flares.

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