Absorption of p-Modes by Slender Magnetic Flux Tubes and p-Mode Lifetimes

Bogdan, T. J.; Hindman, Bradley W.; Cally, Paul Stuart; Charbonneau, Paul

doi:10.1086/177429

Cited by 74 publications

(111 citation statements)

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“…Unfortunately with observations at a single height they were unable to identify what mixture of m = 0, axisymmetric sausage-modes, and m = 1, kinkmodes, they were observing. Theoretical studies of the interaction of flux tubes and waves have been performed in the past, for example Roberts and Webb (1979), Wilson (1980), Spruit (1981), Spruit (1982), Bogdan and Knölker (1989), Solanki (1993), Bogdan et al (1996), Hasan and Kalkofen (1999), Tirry (2000), Gizon, Hanasoge, and Birch (2006), Jain and Gordovskyy (2008), Hanasoge et al (2008), Hanasoge and Cally (2009). It is now well established that slender magnetic flux tubes permit the propagation of the two basic types of magnetohydrodynamic waves: The longitudinal tube waves (sausage modes) with azimuthal wave number m = 0, which are axisymmetric, excited by pressure fluctuations.…”

Section: Introductionmentioning

confidence: 99%

3D Numerical Simulations of f-Mode Propagation Through Magnetic Flux Tubes

et al. 2010

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Three-dimensional numerical simulations have been used to study the scattering of a surface-gravity wave packet by vertical magnetic flux tubes, with radii from 200 km to 3 Mm, embedded in stratified polytropic atmosphere. The scattered wave was found to consist primarily of m = 0 (axisymmetric) and m = 1 modes. It was found that the ratio of the amplitude of these two modes is strongly dependant on the radius of the flux tube: The kink mode is the dominant mode excited in tubes with a small radius while the sausage mode is dominant for large tubes. Simulations of this type provide a simple, efficient and robust way to start understanding the seismic signature of flux tubes, which have recently began to be observed.

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Section: Introductionmentioning

confidence: 99%

3D Numerical Simulations of f-Mode Propagation Through Magnetic Flux Tubes

et al. 2010

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“…The pressure, density and sound speed vary as power laws (see Bogdan et al 1996 for details). Following Bogdan et al (1996), Hindman & Jain (2008) and Jain et al (2009) we set the truncation depth at z = −z 0 352 A. Gascoyne & R. Jain which is our model photosphere where the quantities ρ 0 and P 0 are the values of the mass density and gas pressure at this depth. Above the truncation depth z > −z 0 we assume the existence of a hot vacuum (ρ ext → 0 with temperature T ext → ∞).…”

Section: Equilibrium Configurationmentioning

confidence: 99%

“…For these thin magnetic flux tubes, the lateral variation of the magnetic field across the tube is ignored and the plasma β is constant with depth (see Bogdan et al 1996 andJain 2008 for details).…”

Section: Equilibrium Configurationmentioning

confidence: 99%

“…In this paper we will also ignore the kink waves and specifically concentrate on the m = 0 mode (m being the azimuthal order). Using the formulation of Jain et al (2009) (see also Jain 2008 andBogdan et al 1996), the fluid displacement due to the excitation of sausage waves within the tube can be described by the following equation,…”

Section: The Governing Wave Equationsmentioning

confidence: 99%

“…Also, it is found that the absorption is frequency dependent. Thus, the importance of sub-surface field structure in modifying the properties of f-and p-modes has been realised and many theoretical investigations have concentrated on understanding the physical mechanism responsible for this absorption (e.g., Spruit 1991;Bogdan & Cally 1995;Bogdan et al 1996;Crouch & Cally 2005;Hindman & Jain 2008;Jain et al 2009).…”

Section: Introductionmentioning

confidence: 99%

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Damping rates of p-modes by an ensemble of randomly distributed thin magnetic flux tubes

Gascoyne

Jain

2010

Proc. IAU

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Abstract. The magnetohydrodynamic (MHD) sausage tube waves are excited in the magnetic flux tubes by p-mode forcing. These tube waves thus carry energy away from the p-mode cavity which results in the deficit of incident p-mode energy. We calculate the loss of incident p-mode energy as a damping rate of f-and p-modes. We calculate the damping rates of f-and p-modes by a model Sun consisting of an ensemble of many thin magnetic flux tubes with varying plasma properties and distributions. Each magnetic flux tube is modelled as axisymmetric, vertically oriented and untwisted. We find that the magnitude and the form of the damping rates are sensitive to the plasma-β of the tubes and the upper boundary condition used.

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SLiM: a code for the simulation of wave propagation through an inhomogeneous, magnetised solar atmosphere

2007

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In this paper we describe the semi-spectral linear MHD (SLiM) code which we have written to follow the interaction of linear waves through an inhomogeneous three-dimensional solar atmosphere. The background model allows almost arbitrary perturbations of density, temperature, sound speed as well as magnetic and velocity fields. We give details of several of the tests we have used to check the code. The code will be useful in understanding the helioseismic signatures of various solar features, including sunspots.

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Absorption of p-Modes by Slender Magnetic Flux Tubes and p-Mode Lifetimes

Cited by 74 publications

References 0 publications

3D Numerical Simulations of f-Mode Propagation Through Magnetic Flux Tubes

3D Numerical Simulations of f-Mode Propagation Through Magnetic Flux Tubes

Damping rates of p-modes by an ensemble of randomly distributed thin magnetic flux tubes

SLiM: a code for the simulation of wave propagation through an inhomogeneous, magnetised solar atmosphere

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