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25 April 2024 |
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Three-dimensional structure of a sunspot light bridge | | T. Felipe
; M. Collados
; E. Khomenko
; C. Kuckein
; A. Asensio Ramos
; H. Balthasar
; T. Berkefeld
; C. Denker
; A. Feller
; M. Franz
; A. Hofmann
; C. Kiess
; A. Lagg
; H. Nicklas
; D. Orozco Suárez
; A. Pastor Yabar
; R. Rezaei
; R. Schlichenmaier
; D. Schmidt
; W. Schmidt
; M. Sigwarth
; M. Sobotka
; S. K. Solanki
; D. Soltau
; J. Staude
; K. G. Strassmeier
; R. Volkmer
; O. von der Lühe
; T. Waldmann
; | | Date: |
15 Nov 2016 | | Abstract: | Active regions are the most prominent manifestations of solar magnetic
fields; their generation and dissipation are fundamental problems in solar
physics. Light bridges are commonly present during sunspot decay, but a
comprehensive picture of their role in the removal of photospheric magnetic
field is still missing. We study the three dimensional configuration of a
sunspot and in particular its light bridge during one of the last stages of its
decay. We present the magnetic and thermodynamical stratification inferred from
full Stokes inversions of the photospheric Si I 10827 AA and Ca I 10839 AA
lines obtained with the GREGOR Infrared Spectrograph of the GREGOR telescope at
Observatorio del Teide, Tenerife, Spain. The analysis is complemented by a
study of continuum images covering the disk passage of the active region, which
are provided by the Helioseismic and Magnetic Imager on board the Solar
Dynamics Observatory. The sunspot shows a light bridge with penumbral continuum
intensity that separates the central umbra from a smaller umbra. We find that
in this region the magnetic field lines form a canopy with lower magnetic field
strength in the inner part. The photospheric light bridge is dominated by gas
pressure (high-$eta$), as opposed to the surrounding umbra where the magnetic
pressure is higher. A convective flow is observed in the light bridge. This
flow is able to bend the magnetic field lines and to produce field reversals.
The field lines close above the light bridge and become as vertical and strong
as in the surrounding umbra. We conclude that it develops because of two highly
magnetized regions which come closer during the sunspot evolution. | | Source: | arXiv, 1611.4803 | | Services: | Forum | Review | PDF | Favorites | |
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