Bibcode
Requerey, I. S.; Ruiz Cobo, B.; Del Toro Iniesta, J. C.; Orozco Suárez, D.; Blanco Rodríguez, J.; Solanki, S. K.; Barthol, P.; Gandorfer, A.; Gizon, L.; Hirzberger, J.; Riethmüller, T. L.; van Noort, M.; Schmidt, W.; Martínez Pillet, V.; Knölker, M.
Bibliographical reference
The Astrophysical Journal Supplement Series, Volume 229, Issue 1, article id. 15, 5 pp. (2017).
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3
2017
Citations
5
Refereed citations
5
Description
We study the dynamics and topology of an emerging magnetic flux
concentration using high spatial resolution spectropolarimetric data
acquired with the Imaging Magnetograph eXperiment on board the sunrise
balloon-borne solar observatory. We obtain the full vector magnetic
field and the line of sight (LOS) velocity through inversions of the Fe
i line at 525.02 nm with the SPINOR code. The derived vector magnetic
field is used to trace magnetic field lines. Two magnetic flux
concentrations with different polarities and LOS velocities are found to
be connected by a group of arch-shaped magnetic field lines. The
positive polarity footpoint is weaker (1100 G) and displays an upflow,
while the negative polarity footpoint is stronger (2200 G) and shows a
downflow. This configuration is naturally interpreted as a siphon flow
along an arched magnetic flux tube.
Related projects
Solar and Stellar Magnetism
Magnetic fields are at the base of star formation and stellar structure and evolution. When stars are born, magnetic fields brake the rotation during the collapse of the mollecular cloud. In the end of the life of a star, magnetic fields can play a key role in the form of the strong winds that lead to the last stages of stellar evolution. During
Tobías
Felipe García