Influence of random magnetic field on solar global oscillations: The
incompressible <i>f</i>-mode

Erdélyi, R.; Kerekes, A.; Mole, N.

doi:10.1051/0004-6361:20041456

Cited by 21 publications

(16 citation statements)

References 12 publications

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“…In an earlier study (Erdélyi, Kerekes, and Mole (2005) -hereafter EKM), we have examined the effect of a random atmospheric magnetic field on the solar f mode. The random flow in the present model (representing granular flows) and the random magnetic field of EKM (representing the solar magnetic carpet) was described with the same horizontal and vertical profiles, but on the opposite sides of the interface z = 0.…”

Section: Comparison With Random Magnetic Modelsmentioning

confidence: 99%

Effects of Random Flows on the Solar f Mode: II. Horizontal and Vertical Flow

2008

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We study the influence of horizontal and vertical random flows on the solar f mode in a plane-parallel, incompressible model that includes a static atmosphere. The incompressible limit is an adequate approximation for f -mode type of surface waves that are highly incompressible. The paper revisits and extends the problem investigated earlier by Murawski and Roberts (Astron. Astrophys. 272, 601, 1993).We show that the consideration of the proposed velocity profile requires several restrictive assumptions to be made. These constraints were not recognised in previous studies. The impact of the inconsistencies in earlier modelling is analysed in detail. Corrections to the dispersion relation are derived and the relevance of these corrections is analysed. Finally, the importance of the obtained results is investigated in the context of recent helioseismological data. Detailed comparison with our complementary studies on random horizontal flows (Mole, Kerekes, and Erdélyi, Solar Phys., accepted, 2008) and the random magnetic model of Mole (Astron. Astrophys. 431, 1083, 2005) is also given. In particular, for realistic solar parameters we find significant frequency reduction and wave damping, both of which increase with the characteristic thickness of the random layer.

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Section: Comparison With Random Magnetic Modelsmentioning

confidence: 99%

Effects of Random Flows on the Solar f Mode: II. Horizontal and Vertical Flow

2008

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“…Cally 2006;Schunker & Cally) and they also change locally the elasticity properties of the plasma (e.g. Campbell & Roberts 1989;Erdélyi et al 2005;Erdélyi & Taroyan 2001;Jain & Roberts 1994;Taroyan 2003). Flows, on the other hand will Doppler-shift the frequencies of global oscillations and may shorten/lengthen the travel times of the modes (e.g.…”

Section: Effect Of Magnetic Coupling On Solar Global Oscillationsmentioning

confidence: 99%

Leakage of photospheric motions into the magnetic solar atmosphere: new prospects of magneto‐seismology

Erdélyi¹,

Pintér

Malins

2007

Astron Nachr

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The leakage and coupling of solar global oscillations to the overlaying magnetized solar atmosphere is investigated in this paper. Solar global acoustic oscillations may couple through resonant absorption to atmospheric local magnetic eigenoscillations (i) resulting in small shifts of the order of µHz in the real part of their frequencies as compared to their non-magnetic counterparts, and (ii) causing dissipation of wave energy and a consequent line broadening of the modes. Alternatively, global modes may also penetrate deeply into the magnetized solar atmosphere through leakage along magnetic field lines causing small-scale structuring in the transition region and low corona. By analyzing the dynamic fragmentation generated by direct wave propagations, one may deduce diagnostic information about the geometric and physical properties of the local magnetic environment in the atmosphere. A few numerical examples are presented here to demonstrate the leakage of global oscillations and its influence and omnipotence on the dynamics of the lower solar atmosphere.

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“…For modelling effects of stochastic magnetic fields see Erdélyi, Kerekes, and Mole (2005) and Mole (2008a, 2008b).…”

Section: Introductionmentioning

confidence: 99%

Modelling the Coupling Role of Magnetic Fields in Helioseismology

Pintér

2008

Sol Phys

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Helioseismic global modes change in time, in particular on time scales of the solar cycle. These changes show, in fact, strong correlation with the magnetic activity cycle of the Sun, indicating that a most likely cause of the variation of the mode characteristics, such as frequency, is the magnetic field. In the present paper I attempt to find out in what ways and to what degree the magnetic atmosphere of the Sun can influence the f and p modes of helioseismology. Frequency shifts of the order of a microhertz, line widths of the order of a nanohertz, and penetration depths of the order of a megameter are obtained.

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Influence of random magnetic field on solar global oscillations: The incompressible f-mode

Cited by 21 publications

References 12 publications

Effects of Random Flows on the Solar f Mode: II. Horizontal and Vertical Flow

Effects of Random Flows on the Solar f Mode: II. Horizontal and Vertical Flow

Leakage of photospheric motions into the magnetic solar atmosphere: new prospects of magneto‐seismology

Modelling the Coupling Role of Magnetic Fields in Helioseismology

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