Where the Granular Flows Bend

Bibcode
2010ApJ...723L.159K
DOI
10.1088/2041-8205/723/2/L159
Khomenko, E.; Martínez-Pillet, V.; Solanki, S. K.; del Toro Iniesta, J. C.; Gandorfer, A.; Bonet, J. A.; Domingo, V.; Schmidt, W.; Barthol, P.; Knölker, M.
Bibliographical reference

The Astrophysical Journal Letters, Volume 723, Issue 2, pp. L159-L163 (2010).

Advertised on:
11
2010
Number of authors
10
IAC number of authors
3
Citations
12
Refereed citations
10
Description
Based on IMaX/SUNRISE data, we report on a previously undetected phenomenon in solar granulation. We show that in a very narrow region separating granules and intergranular lanes, the spectral line width of the Fe I 5250.2 Å line becomes extremely small. We offer an explanation of this observation with the help of magneto-convection simulations. These regions with extremely small line widths correspond to the places where the granular flows bend from upflow in granules to downflow in intergranular lanes. We show that the resolution and image stability achieved by IMaX/SUNRISE are important requisites to detect this interesting phenomenon.
Related projects
Project Image
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
In progress
Type
Refereed
Solar Physics (FS)

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