Supersonic downflows in the vicinity of a growing pore. Evidence of unresolved magnetic fine structure at chromospheric heights

Details Supersonic downflows in the vicinity of a growing pore. Evidence of unresolved magnetic fine structure at chromospheric heights Supersonic downflows in the vicinity of a growing pore. Evidence of unresolved magnetic fine structure at chromospheric heights

Feb 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007a%26a...462.1147l&link_type=abstract

Astronomy and Astrophysics, Volume 462, Issue 3, February II 2007, pp.1147-1155

Astronomy and Astrophysics

Astrophysics

18

Sun: Chromosphere, Sun: Magnetic Fields, Sun: Infrared

Scientific paper

Aims:The velocity and magnetic fine structure of the chromosphere at the leg of an emerging magnetic loop is investigated at a location of supersonic downflows. Methods: We analyze a time series of spectropolarimetric data in the He i 1083 nm triplet covering a time interval of ≈70 min. The temporal evolution as well as the topology of the magnetic field in the downflow region are investigated. We apply an inversion technique based on a genetic algorithm using the Milne-Eddington approach. The technique is very reliable and robust in retrieving maps of the velocity and the magnetic field vector for both atmospheric components separately. Results: We observe redshifts corresponding to a downflow speed of up to 40 km s-1 in the vicinity of a growing pore. These supersonic downflows always coexist with a second atmospheric component almost at rest (slow component) within the same resolution element. The redshifted component is more inclined to the solar normal than the slow component and has a different field strength. Conclusions: .We interpret this downflow as a consequence of the draining of the rising loops. The different magnetic field orientation of the redshifted and the slow component give rise to two possible interpretations: an uncombed structure of the chromosphere, similar to the differently inclined flux-tubes in the penumbra of a sunspot, or a cloud-like structure containing gas at different velocities in two separate height layers of the solar atmosphere.

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