Heating Diagnostics with MHD Waves

Taroyan, Y.; Erdélyi, R.

doi:10.1007/s11214-009-9506-9

Cited by 82 publications

(64 citation statements)

References 122 publications

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“…A recent study by Antolin & Shibata [40] investigates heating based on torsional Alfvén waves and suggests that, within the constraints of their 1.5 D model, this mechanism is viable only in a rather narrow regime, requiring long and thick loops (see Jess et al [41] for a possible observational identification of torsional Alfvén waves in the solar chromosphere). We refer the interested reader to Taroyan & Erdélyi [42] for a review of heating diagnostics with MHD waves.…”

Section: Acoustic and Magnetohydrodynamic Wavesmentioning

confidence: 99%

A contemporary view of coronal heating

Parnell

Moortel

2012

Phil. Trans. R. Soc. A.

211

188

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Determining the heating mechanism (or mechanisms) that causes the outer atmosphere of the Sun, and many other stars, to reach temperatures orders of magnitude higher than their surface temperatures has long been a key problem. For decades, the problem has been known as the coronal heating problem, but it is now clear that 'coronal heating' cannot be treated or explained in isolation and that the heating of the whole solar atmosphere must be studied as a highly coupled system. The magnetic field of the star is known to play a key role, but, despite significant advancements in solar telescopes, computing power and much greater understanding of theoretical mechanisms, the question of which mechanism or mechanisms are the dominant supplier of energy to the chromosphere and corona is still open. Following substantial recent progress, we consider the most likely contenders and discuss the key factors that have made, and still make, determining the actual (coronal) heating mechanism (or mechanisms) so difficult.

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Section: Acoustic and Magnetohydrodynamic Wavesmentioning

confidence: 99%

A contemporary view of coronal heating

Parnell

Moortel

2012

Phil. Trans. R. Soc. A.

211

188

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“…The highly dynamic solar photosphere is a rich source of waves, which are believed to be one of the plausible candidates responsible for heating the upper solar atmosphere (see a recent review by Taroyan & Erdélyi 2009, in this context). Magnetic fields and magnetohydrodynamic (MHD) waves play an important role in the solar atmosphere's energy budget.…”

Section: Introductionmentioning

confidence: 99%

Three-Dimensional Simulations of Magnetohydrodynamic Waves in Magnetized Solar Atmosphere

Vigeesh

Fedun

Hasan

et al. 2012

ApJ

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We present results of three-dimensional numerical simulations of magnetohydrodynamic (MHD) wave propagation in a solar magnetic flux tube. Our study aims at understanding the properties of a range of MHD wave modes generated by different photospheric motions. We consider two scenarios observed in the lower solar photosphere, namely, granular buffeting and vortex-like motion, among the simplest mechanism for the generation of waves within a strong, localized magnetic flux concentration. We show that granular buffeting is likely to generate stronger slow and fast magnetoacoustic waves as compared to swirly motions. Correspondingly, the energy flux transported differs as a result of the driving motions. We also demonstrate that the waves generated by granular buffeting are likely to manifest in stronger emission in the chromospheric network. We argue that different mechanisms of wave generation are active during the evolution of a magnetic element in the intergranular lane, resulting in temporally varying emission at chromospheric heights.

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“…The studies of recently reported observed ubiquitous wave motions in a range of magCorrespondence to: V. Fedun (v.fedun@sheffield.ac.uk) netic field configurations in the photosphere, chromosphere and corona are of particular interest, since through different mechanisms of wave damping they might be responsible for the heating of the solar plasma (see e.g. Banerjee et al, 2007;Taroyan and Erdélyi, 2009). Furthermore, one can exploit these waves by the technique of solar magneto-seismology to probe the fine structure of the Sun's magnetised and highly dynamic atmosphere (see e.g.…”

Section: Introductionmentioning

confidence: 99%

MHD waves generated by high-frequency photospheric vortex motions

et al. 2011

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Abstract.In this paper, we discuss simulations of MHD wave generation and propagation through a threedimensional open magnetic flux tube in the lower solar atmosphere. By using self-similar analytical solutions for modelling the magnetic field in Cartesian coordinate system, we have constructed a 3-D magnetohydrostatic configuration which is used as the initial condition for non-linear MHD wave simulations. For a driver we have implemented a highfrequency vortex-type motion at the footpoint region of the open magnetic flux tube. It is found that the implemented swirly source is able to excite different types of wave modes, i.e. sausage, kink and torsional Alfvén modes. Analysing these waves by magneto-seismology tools could provide insight into the magnetic structure of the lower solar atmosphere.

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Heating Diagnostics with MHD Waves

Cited by 82 publications

References 122 publications

A contemporary view of coronal heating

A contemporary view of coronal heating

Three-Dimensional Simulations of Magnetohydrodynamic Waves in Magnetized Solar Atmosphere

MHD waves generated by high-frequency photospheric vortex motions

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