It is a well-known result that the power of five-minute oscillations is progressively reduced by magnetic fields in the solar photosphere. Many authors have pointed out that this could be due to a complex interaction of many processes: opacity effects, MHD mode conversion, and intrinsically weaker acoustic emissivity in strong magnetic fields. While five-minute oscillations predominate in the photosphere, it has been shown that in the chromosphere three-minute oscillations are more common. Two main theories have been proposed to explain the presence of the latter oscillations based upon resonance filtering in the atmospheric cavity and non-linear interactions. In this work, we show, through the analysis of IBIS observations of a solar pore in the photospheric Fe I 617.3 nm line, that three-minute waves are already present at the height of formation of this line, their amplitude depends on the magnetic field strength, and they are strictly confined to the umbral region.

Stangalini, M., Giannattasio, F., DEL MORO, D., Berrilli, F. (2012). Three-minute wave enhancement in the solar photosphere. ASTRONOMY & ASTROPHYSICS [10.1051/0004-6361/201118654].

Three-minute wave enhancement in the solar photosphere

DEL MORO, DARIO;BERRILLI, FRANCESCO
2012-03-01

Abstract

It is a well-known result that the power of five-minute oscillations is progressively reduced by magnetic fields in the solar photosphere. Many authors have pointed out that this could be due to a complex interaction of many processes: opacity effects, MHD mode conversion, and intrinsically weaker acoustic emissivity in strong magnetic fields. While five-minute oscillations predominate in the photosphere, it has been shown that in the chromosphere three-minute oscillations are more common. Two main theories have been proposed to explain the presence of the latter oscillations based upon resonance filtering in the atmospheric cavity and non-linear interactions. In this work, we show, through the analysis of IBIS observations of a solar pore in the photospheric Fe I 617.3 nm line, that three-minute waves are already present at the height of formation of this line, their amplitude depends on the magnetic field strength, and they are strictly confined to the umbral region.
mar-2012
Pubblicato
Rilevanza internazionale
Articolo
Esperti anonimi
Settore FIS/05 - ASTRONOMIA E ASTROFISICA
English
MAGNETIC-FIELD; P-MODES; OSCILLATIONS; ATMOSPHERE; SUNSPOTS; SPECTROSCOPY; CHROMOSPHERE; PROPAGATION; IBIS
http://www.aanda.org/articles/aa/abs/2012/03/aa18654-11/aa18654-11.html
Stangalini, M., Giannattasio, F., DEL MORO, D., Berrilli, F. (2012). Three-minute wave enhancement in the solar photosphere. ASTRONOMY & ASTROPHYSICS [10.1051/0004-6361/201118654].
Stangalini, M; Giannattasio, F; DEL MORO, D; Berrilli, F
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/2108/77413
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