MHD Waves in the Solar Wind

Ofman, L.

doi:10.1002/9781119055006.ch14

Cited by 4 publications

(3 citation statements)

References 80 publications

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“…This mechanism is efficient in the presence of large transverse density inhomogeneity such as that produced by the PDI. The effects of phase mixing on the dissipation of Alfvén waves due to background inhomogeneity in coronal holes were studied using 2.5D MHD and theoretical models in the past (see the reviews Ofman, 2005. One of the first fully self consistent models of fast solar wind acceleration by Alfvén waves in a transversely inhomogeneous medium in 2.5D MHD was carried out by Matsumoto & Suzuki (2012).…”

Section: Theoretical Modellingmentioning

confidence: 99%

Magnetohydrodynamic Waves in Open Coronal Structures

et al. 2021

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Modern observatories have revealed the ubiquitous presence of magnetohydrodynamic waves in the solar corona. The propagating waves (in contrast to the standing waves) are usually originated in the lower solar atmosphere which makes them particularly relevant to coronal heating. Furthermore, open coronal structures are believed to be the source regions of solar wind, therefore, the detection of MHD waves in these structures is also pertinent to the acceleration of solar wind. Besides, the advanced capabilities of the current generation telescopes have allowed us to extract important coronal properties through MHD seismology. The recent progress made in the detection, origin, and damping of both propagating slow mangetoacoustic waves and kink (Alfvénic) waves is presented in this review article especially in the context of open coronal structures. Where appropriate, we give an overview on associated theoretical modelling studies. A few of the important seismological applications of these waves are discussed. The possible role of Aflvénic waves in the acceleration of solar wind is also touched upon.

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Section: Theoretical Modellingmentioning

confidence: 99%

Magnetohydrodynamic Waves in Open Coronal Structures

et al. 2021

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“…This mechanism is efficient in the presence of large transverse density inhomogeneity such as that produced by the PDI. The effects of phase mixing on the dissipation of Alfvén waves due to background inhomogeneity in coronal holes were studies using 2.5D MHD and theoretical models in the past(see the reviews Ofman (2005). One of the first fully self consistent models of fast solar wind acceleration by Alfvén waves in 2.5D MHD was carried out by Matsumoto & Suzuki (2012).…”

Section: Theoretical Modellingmentioning

confidence: 99%

MHD Waves in open coronal structures

Banerjee,

Prasad,

Pant

et al. 2020

Preprint

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“…Kleindienst et al, 2009;Delamere, 2016). ULF waves have also been found to be embedded in the solar wind flow, from the inner heliosphere out to the ice giants (Zhang et al, 1991;Ofman, 2016). The prevalence of these embedded periods also appears to vary with the solar cycle, though work towards a detailed understanding of this is ongoing (Hynönen, R., Tanskanen, E. I., and Francia, P., 2020).…”

Section: Ultra-low-frequency Waves In Space Plasmasmentioning

confidence: 99%

The Pulsating Magnetosphere at Jupiter

Manners¹,

Masters²

2020

Preprint

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The magnetosphere of Jupiter is the largest planetary magnetosphere in the solar system, and plays host to internal dynamics that remain, in many ways, mysterious. Prominent among these mysteries are the ultra-low-frequency (ULF) pulses ubiquitous in this system. Pulsations in the electromagnetic emissions, magnetic field and flux of energetic particles have been observed for decades, with little to indicate the source mechanism. While ULF waves have been observed in the magnetospheres of all the magnetized planets, the magnetospheric environment at Jupiter seems particularly conducive to the emergence of ULF waves over a wide range of periods (1-100+ minutes). This is mainly due to the high variability of the system on a global scale: internal plasma sources and a powerful intrinsic magnetic field produce a highly-compressible magnetospheric cavity, which can be reduced to a size significantly smaller than its nominal expanded state by variations in the dynamic pressure of the solar wind. Compressive fronts in the solar wind, turbulent surface interactions on the magnetopause and internal plasma processes can also all lead to ULF wave activity inside the magnetosphere.To gain the first comprehensive view of ULF waves in the Jovian system, we have performed a heritage survey of magnetic field data measured by six spacecraft that visited the magnetosphere (Galileo, Ulysses, Voyager 1 & 2 and Pioneer 10 & 11). We found several-hundred wave events consisting of wave packets parallel or transverse to the mean magnetic field, interpreted as fast-mode or Alfv&#233;nic MHD wave activity, respectively. Parallel and transverse events were often coincident in space and time, which may be evidence of global Alfv&#233;nic resonances of the magnetic field known as field-line-resonances. We found that 15-, 30- and 40-minute periods dominate the Jovian ULF wave spectrum, in agreement with the dominant &#8220;magic frequencies&#8221; often reported in existing literature.We will discuss potential driving mechanisms as informed by the results of the heritage survey, how this in turn affects our understanding of energy transfer in the magnetosphere, and potential investigations to be made using data from the JUNO spacecraft. We will also discuss the potential for multiple resonant cavities, and how the resonance modes of the Jovian magnetosphere may differ from those of the other magnetized planets.

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MHD Waves in the Solar Wind

Cited by 4 publications

References 80 publications

Magnetohydrodynamic Waves in Open Coronal Structures

Magnetohydrodynamic Waves in Open Coronal Structures

MHD Waves in open coronal structures

The Pulsating Magnetosphere at Jupiter

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