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.
Referencia bibliográfica

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

Fecha de publicación:
11
2010
Número de autores
10
Número de autores del IAC
3
Número de citas
13
Número de citas referidas
11
Descripción
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.
Proyectos relacionados
Imagen del Proyecto
Magnestismo Solar y Estelar
Los campos magnéticos son uno de los ingredientes fundamentales en la formación de estrellas y su evolución. En el nacimiento de una estrella, los campos magnéticos llegan a frenar su rotación durante el colapso de la nube molecular, y en el fin de la vida de una estrella, el magnetismo puede ser clave en la forma en la que se pierden las capas
Tobías
Felipe García
En ejecución
Tipo
Con árbitro
Física Solar (FS)

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