The heating of the solar corona by the resonant absorption of alfven waves

Alkahby, Hadi Y.; Hussain, T M

doi:10.1016/0893-9659(93)90079-3

Cited by 6 publications

(3 citation statements)

References 8 publications

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“…On the other hand the importance of the magnetic field and the dissipation of Alfvn waves in the heating process of the solar atmosphere is being increasingly recognized see Alkahby 1993aAlkahby , 1993bAlkahby , 1993c ], Yanowitch 1989, 1991], Eltayeb 1970], Moffatt [197} ], Priest 1984 ], Robert [1968] Webb [1980 ], Zhughda and Dzhalilov [1986 for references). In fact recent investigation emphasizes the influence of the vertical magnetic field and its role in the heating process of the solar atmosphere.…”

Section: Introductionmentioning

confidence: 99%

On resistive dissipation of Alfvén waves in an isothermal atmosphere

Alkahby

1996

International Journal of Mathematics and Mathematical Sciences

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In this paper we will examine the reflection and dissipation of Alfvén waves, resulting from a uniform vertical magnetic field, in an inviscid, resistive and isothermal atmosphere. An equation for the damping length distance that wave can travel at Alfvén speed is derived. This equation shows that the damping length is proportional to the wave number and the density scale height and it is valid not only for Alfvén waves but also for any wave that travels at Alfvén speed. Moreover, it is shown that the atmosphere may be divided into two distinct regions connected by an absorbing and reflecting transition region. In the lower region the solution can be represented as a linear combination of two, incident and reflected, propagating waves with the same wavelengths and the same dissipative factors. In the upper region the effect of the resistive diffusivity and Alfvén speed is large and the solution, which satisfies the prescribed boundary conditions, either decays with altitude or behaves as a constant. In the transition region the reflection, dissipation and absorption of the magnetic energy of the waves take place. The reflection coefficient, the dissipative factors, which are proportional to the damping length, are determined and the conclusions are discussed in connection with heating of the solar atmosphere.

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Section: Introductionmentioning

confidence: 99%

On resistive dissipation of Alfvén waves in an isothermal atmosphere

Alkahby

1996

International Journal of Mathematics and Mathematical Sciences

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“…The resonance occurs if the magnetic field strength is matched with wave length of the wave for infinitely many values of the magnetic field and the frequency of the wave [1,3,4,6,7,8] and a numerical computation can be found in [4,5]. At the resonance frequencies the values of the kinetic and magnetic energies of the wave will be increase to a very large values.…”

Section: Asymptotic Estimate and The Magnitude Of The Reflection Coefmentioning

confidence: 99%

“…The motivation of these studies is due mainly to the application of these waves to phenomena in compressible ionized fluids such as solar, stellar, and planetary atmospheres and to certain phenomena in ocean dynamics (see [1,2,3,7,9,10,11,12,13] and the references therein). In this paper, a linearized theory of magnetoatmospheric waves, involving the combined effect of restoring forces due to compressibility, magnetic pressure, and radiative damping is developed for the case of a uniform horizontal magnetic field.…”

Section: Introductionmentioning

confidence: 99%

Effect of the radiative damping on magnetohydrodynamic waves in an isothermal medium

Alkahby

Talmadge

Jalbout

2002

International Journal of Mathematics and Mathematical Sciences

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We investigate the effect of the heat radiation on the reflection and dissipation of upward propagating waves in an isothermal atmosphere. It is shown that the magnetic field produces a totally reflecting layer. Consequently, the atmosphere can be divided into two distinct regions. In the lower region, the solution can be written as a linear combination of an upward and a downward propagating wave, and in the upper region the solution, which satisfies the upper boundary condition, decays exponentially or behaves like a constant. These two regions are connected by a region in which the reflection and transmission of the waves takes place. Moreover, the heat radiation affects only the lower region and changes the sound speed from the adiabatic value to the isothermal one. The reflection coefficient and the attenuation factor of the amplitude of the waves are derived for all values of the heat radiation coefficient. Finally, the conclusions are presented in connection with the heating process of the solar atmosphere.2000 Mathematics Subject Classification: 76N15.

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The dissipation of magneto-acoustic waves

Alkahby

1994

Computers & Mathematics with Applications

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The heating of the solar corona by the resonant absorption of alfven waves

Cited by 6 publications

References 8 publications

On resistive dissipation of Alfvén waves in an isothermal atmosphere

On resistive dissipation of Alfvén waves in an isothermal atmosphere

Effect of the radiative damping on magnetohydrodynamic waves in an isothermal medium

The dissipation of magneto-acoustic waves

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