Dependence of sunspot photospheric waves on the depth of the source of solar p-modes

Bibcode
2017A&A...599L...2F
DOI
10.1051/0004-6361/201630123
Felipe, T.; Khomenko, E.
Bibliographical reference

Astronomy and Astrophysics, Volume 599, id.L2, 4 pp.

Advertised on:
2
2017
Journal
Astronomy and Astrophysics
Number of authors
2
IAC number of authors
2
Citations
10
Refereed citations
10
Description
Photospheric waves in sunspots moving radially outward at speeds faster than the characteristic wave velocities have been recently detected. It has been suggested that they are the visual pattern of p-modes excited around 5 Mm beneath the sunspot's surface. Using numerical simulations, we performed a parametric study of the waves observed at the photosphere and higher layers that were produced by sources located at different depths beneath the sunspot's surface. The observational measurements are consistent with waves driven between approximately 1 Mm and 5 Mm below the sunspot's surface.
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Numerical simulation through complex computer codes has been a fundamental tool in physics and technology research for decades. The rapid growth of computing capabilities, coupled with significant advances in numerical mathematics, has made this branch of research accessible to medium-sized research centers, bridging the gap between theoretical and

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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
Methods
Helioseismology
Sunspots
Solar Physics (FS)

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