Fast-to-Alfvén Mode Conversion Mediated by Hall Current. II. Application to the Solar Atmosphere

P. A. González-Morales, E. Khomenko, P. S. Cally

Research output: Contribution to journalArticleResearchpeer-review

1 Citation (Scopus)

Abstract

Coupling between fast magnetoacoustic and Alfvén waves can be observed in fully ionized plasmas mediated by stratification and 3D geometrical effects. In Paper I, Cally & Khomenko have shown that in a weakly ionized plasma, such as the solar photosphere and chromosphere, the Hall current introduces a new coupling mechanism. The present study extends the results from Paper I to the case of warm plasma. We report on numerical experiments where mode transformation is studied using quasi-realistic stratification in thermodynamic parameters resembling the solar atmosphere. This redresses the limitation of the cold plasma approximation assumed in Paper I, in particular allowing the complete process of coupling between fast and slow magnetoacoustic modes and subsequent coupling of the fast mode to the Alfvén mode through the Hall current. Our results confirm the efficacy of the mechanism proposed in Paper I for the solar case. We observe that the efficiency of the transformation is a sensitive function of the angle between the wave propagation direction and the magnetic field, and of the wave frequency. The efficiency increases when the field direction and the wave direction are aligned for increasing wave frequencies. After scaling our results to typical solar values, the maximum amplitude of the transformed Alfvén waves, for a frequency of 1 Hz, corresponds to an energy flux (measured above the height of peak Hall coupling) of ∼103 W m-2, based on an amplitude of 500 m s-1 at β = 1, which is sufficient to play a major role in both quiet and active region coronal heating.

Original languageEnglish
Article number94
Number of pages12
JournalAstrophysical Journal
Volume870
Issue number2
DOIs
Publication statusPublished - 10 Jan 2019

Keywords

  • magnetohydrodynamics (MHD)
  • Sun: chromosphere
  • Sun: magnetic fields
  • Sun: oscillations
  • waves

Cite this

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abstract = "Coupling between fast magnetoacoustic and Alfv{\'e}n waves can be observed in fully ionized plasmas mediated by stratification and 3D geometrical effects. In Paper I, Cally & Khomenko have shown that in a weakly ionized plasma, such as the solar photosphere and chromosphere, the Hall current introduces a new coupling mechanism. The present study extends the results from Paper I to the case of warm plasma. We report on numerical experiments where mode transformation is studied using quasi-realistic stratification in thermodynamic parameters resembling the solar atmosphere. This redresses the limitation of the cold plasma approximation assumed in Paper I, in particular allowing the complete process of coupling between fast and slow magnetoacoustic modes and subsequent coupling of the fast mode to the Alfv{\'e}n mode through the Hall current. Our results confirm the efficacy of the mechanism proposed in Paper I for the solar case. We observe that the efficiency of the transformation is a sensitive function of the angle between the wave propagation direction and the magnetic field, and of the wave frequency. The efficiency increases when the field direction and the wave direction are aligned for increasing wave frequencies. After scaling our results to typical solar values, the maximum amplitude of the transformed Alfv{\'e}n waves, for a frequency of 1 Hz, corresponds to an energy flux (measured above the height of peak Hall coupling) of ∼103 W m-2, based on an amplitude of 500 m s-1 at β = 1, which is sufficient to play a major role in both quiet and active region coronal heating.",
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Fast-to-Alfvén Mode Conversion Mediated by Hall Current. II. Application to the Solar Atmosphere. / González-Morales, P. A.; Khomenko, E.; Cally, P. S.

In: Astrophysical Journal, Vol. 870, No. 2, 94, 10.01.2019.

Research output: Contribution to journalArticleResearchpeer-review

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AU - González-Morales, P. A.

AU - Khomenko, E.

AU - Cally, P. S.

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