Hinode/SOT Observation of Fine Structure of the Evershed Flow

Details Hinode/SOT Observation of Fine Structure of the Evershed Flow Hinode/SOT Observation of Fine Structure of the Evershed Flow

May 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...210.9408i&link_type=abstract

American Astronomical Society Meeting 210, #94.08; Bulletin of the American Astronomical Society, Vol. 39, p.218

Astronomy and Astrophysics

Astronomy

Scientific paper

Small scale structure of the Evershed effect was studied using the Spectropolarimeter (SP) and Broadband Filter Imager (BFI) of SOT aboard Hinode. SP maps and high cadence continuum images of BFI coverting entire sunspots are used to investigate the spatial distribution of the flow field, brightness and magnetic fields. It is revealed that the Evershed flow starts at the front edge of inwardly migrating penumbral grains with an upward velocity component and turns to nearly holizontal flow preferentially in dark lanes (or dark core of filaments) of the penumbra. Our results are in general agreement with the well known uncombed penumbral concept in which the Evershed flow takes place in nearly holizontal field channels. We discovered a number of tiny elongated regions in deep photosphere in which there is an obvious upward motion of 1-1.5km/s distributing over the penumbra.
They could be identified as the 'foot points' of the individual Evershed flow channels. Cross-correlation among the flow speed, intensity, magnetic field strength and inclination, and distribution of string down flows in and around the penumbra will also be discussed.

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