Energy transport in sunspot penumbrae

Details Energy transport in sunspot penumbrae Energy transport in sunspot penumbrae

Apr 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986a%26a...158..351s&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 158, no. 1-2, April 1986, p. 351-360. Research supported by the Max-Planck-Ins

Astronomy and Astrophysics

Astrophysics

37

Energy Transfer, Penumbras, Stellar Models, Sunspots, Pressure Gradients, Solar Flux, Solar Magnetic Field, Solar Prominences

Scientific paper

It is proposed that the magnetic field in the outer penumbra of a sunspot is almost horizontal and that the penumbra itself is very shallow, with a sharp lower boundary. A simple model of energy transport in the outer penumbra predicts that there is a Wilson depression of about 100 km, below which the penumbra extends for only 80 km. A two-component model with bright and dark filaments suggests that the associated differences in observed field strength and corrugations of the visible surface of the penumbra will be small. The authors argue that flows along the field are needed to explain the existence of bright and dark filaments while the Evershed flow is driven by pressure differences along flux tubes.

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