Solar Atmospheric Heating by Hydromagnetic Waves

Piddington, J. H.

doi:10.1093/mnras/116.3.314

Cited by 126 publications

(66 citation statements)

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“…Still Piddington (1956) has shown that an upwardtravelling MHD waves can provide a heating of the solar material in the chromosphere and inner corona. A plausible mechanism, within these conditions, responsible for the excitation of the ionized calcium and fitting observations, is briefly described in Leighton (1959).…”

Section: Data and Analysismentioning

confidence: 99%

On the magnetic field strength in the solar corona

et al. 2004

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Abstract. On the base of the interferometric observations during the total solar eclipse on 11 August 1999 magnetic field strength in a coronal volume at the height of 10 5 km above the solar limb has been evaluated using an indirect method. A cold coronal emission (CCE), seen in the lines of Hα and K CaII, existed there. The conclusion is made that the magnetic field strength in this bulk, before the investigated CCE-region formed, was about 100-200 G.

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Section: Data and Analysismentioning

confidence: 99%

On the magnetic field strength in the solar corona

et al. 2004

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“…The hydromagnetic equations may be listed (Piddington 1954a(Piddington , 1956(Piddington , 1959 period taken to accelerate the neutral atomes to the same velocity as the plasma. Though we are dealing with a partially ionized gas, equation (1) refers to a fully ionized gas because the effects of neutral atomes are introduced separately by equations (2) and (3).…”

Section: The Transmission Equationsmentioning

confidence: 99%

“…Piddington (1956Piddington ( , 1959 provided useful information about the transmission of geomagnetic disturbances by a study of the separate equation of the ion-electron plasma and the neutral atom gas.…”

Section: Introductionmentioning

confidence: 99%

On The Reflection and Refraction of Hydromagnetic Waves in Ionised Gas

Namikawa

1961

J. geomagn. geoelec

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We are interested in the manner of propagation of hydromagnetic waves in the Earth's upper atmosphere. The density changes continuously in the atmosphere and the steady magnetic field is a dipole field, but we discuss here the laws of reflection and refraction of hydromagnetic waves at a plane boundary between two semi-infinite homogeneous media of anisotropic electrical conductivity under a uniform steady magnetic field. When the steady magnetic field is perpendicular to the boundary plane, the laws of reflection and refraction are simple, but when the steady magnetic field makes an angle with the plane, they are complicated. The incident ordinary (or extraordinary) waves may be reflected or refracted as the ordinary or extraordinary waves and propagate anisotropically.

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“…Russell & Fletcher (2013) developed a model of energy transmission as waves propagate beyond the transition region and found strong resistive damping in the chromosphere due to ion-neutral friction, with a strong dependence on frequency. Ion-neutral friction is well established as one of the primary damping mechanisms of Alfvén waves (Piddington 1956), and in recent years the governing theory has received significant attention (Soler et al 2013; Leake et al 2014;Khomenko 2017). The effectiveness of ion-neutral friction depends on the local field strength, and is most efficient when the Lorentz force is strong compared to other dynamic forces .…”

Section: Introductionmentioning

confidence: 99%

A Hydrodynamic Model of Alfvénic Wave Heating in a Coronal Loop and Its Chromospheric Footpoints

Reep

Russell

Tarr

et al. 2018

ApJ

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Alfvénic waves have been proposed as an important energy transport mechanism in coronal loops, capable of delivering energy to both the corona and chromosphere and giving rise to many observed features, of flaring and quiescent regions. In previous work, we established that resistive dissipation of waves (ambipolar diffusion) can drive strong chromospheric heating and evaporation, capable of producing flaring signatures. However, that model was based on a simplified assumption that the waves propagate instantly to the chromosphere, an assumption which the current work removes. Via a ray tracing method, we have implemented traveling waves in a field-aligned hydrodynamic simulation that dissipate locally as they propagate along the field line. We compare this method to and validate against the magnetohydrodynamics code Lare3D. We then examine the importance of travel times to the dynamics of the loop evolution, finding that (1) the ionization level of the plasma plays a critical role in determining the location and rate at which waves dissipate; (2) long duration waves effectively bore a hole into the chromosphere, allowing subsequent waves to penetrate deeper than previously expected, unlike an electron beam whose energy deposition rises in height as evaporation reduces the mean-free paths of the electrons; (3) the dissipation of these waves drives a pressure front that propagates to deeper depths, unlike energy deposition by an electron beam.

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Solar Atmospheric Heating by Hydromagnetic Waves

Cited by 126 publications

References 0 publications

On the magnetic field strength in the solar corona

On the magnetic field strength in the solar corona

On The Reflection and Refraction of Hydromagnetic Waves in Ionised Gas

A Hydrodynamic Model of Alfvénic Wave Heating in a Coronal Loop and Its Chromospheric Footpoints

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