2001
DOI: 10.1086/321641
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Generation of Ion Cyclotron Waves in Coronal Holes by a Global Resonant Magnetohydrodynamic Mode

Abstract: The damping of ion cyclotron waves is a process that can provide e †ective coronal heating and solar wind acceleration. However, the mechanism of generation of these waves in the solar corona remains unclear. We suggest that the ion cyclotron waves in coronal holes are excited by plasma instability that is driven by current Ñuctuations of a global resonant magnetohydrodynamic (MHD) mode. The frequency of the MHD mode is much lower than the proton gyrofrequency, so that its direct cyclotron damping is absent. A… Show more

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Cited by 47 publications
(50 citation statements)
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“…However, in the case of higher wave frequencies, f $ 1 Hz, considered in our model, the reduced reflection makes the turbulence dissipation negligible, as is illustrated by Dmitruk and Matthaeus [2003, Figure 7]. Nonlocal transport due to current instabilities [Markovskii, 2001;Markovskii and Hollweg, 2002] can only be efficient when the MHD waves have strong shear flows or currents. Hence this type of transport requires prestructured Alfvén waves with sufficiently small scales either across the background magnetic field or in the field-aligned direction (which in turn implies already high-frequency Alfvén waves).…”
Section: Introductionmentioning
confidence: 75%
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“…However, in the case of higher wave frequencies, f $ 1 Hz, considered in our model, the reduced reflection makes the turbulence dissipation negligible, as is illustrated by Dmitruk and Matthaeus [2003, Figure 7]. Nonlocal transport due to current instabilities [Markovskii, 2001;Markovskii and Hollweg, 2002] can only be efficient when the MHD waves have strong shear flows or currents. Hence this type of transport requires prestructured Alfvén waves with sufficiently small scales either across the background magnetic field or in the field-aligned direction (which in turn implies already high-frequency Alfvén waves).…”
Section: Introductionmentioning
confidence: 75%
“…The direct turbulent cascade toward higher frequencies [Hollweg, 1986;Tu and Marsch, 1997], and the generation by currents carried by MHD waves [Markovskii, 2001;Markovskii and Hollweg, 2002] have been proposed as local and nonlocal transport mechanisms of wave energy to the ion-cyclotron dissipation range. However, under the solar corona conditions the turbulent cascade is anisotropic and proceeds toward high cross-field wave numbers rather than to high field-aligned wave numbers required for ion-cyclotron resonance .…”
Section: Introductionmentioning
confidence: 99%
“…The ion cyclotron resonance and the ion cyclotron mode have been discussed in the context of problems related to the heating of the solar corona, e.g., Marsch et al (1982), Cranmer et al (1999), Cranmer (2000), Tu & Marsch (2001), Markovskii (2001), Isenberg (2001), Hollweg & Isenberg (2002). This is due to various reasons, such as the evidence obtained from in situ measurements in the solar wind and coronal holes of resonant ion cyclotron heating (Hollweg & Isenberg 2002), and a preferential heating of coronal ions (with respect to electrons) which is most dominant in the direction perpendicular to the magnetic field lines.…”
Section: Introductionmentioning
confidence: 99%
“…We need to compare the energy budget of the solar wind and the threshold of the instability. At the coronal base the degree of intermittency turns out to be around several hundred (Markovskii andHollweg, 2002b, 2003).…”
Section: Basic Conceptsmentioning
confidence: 99%
“…Alternatively, the ion cyclotron waves can be excited by the plasma instability driven by currents associated with a global MHD mode (Markovskii, 2001). A similar idea was used by Viñas et al (2000) to explain electron heating in the corona.…”
Section: Introductionmentioning
confidence: 99%