An Observational Manifestation of Magnetoatmospheric Waves in Internetwork Regions of the Chromosphere and Transition Region

McIntosh, Scott W.; Bogdan, Thomas J.; Cally, Paul Stuart; Carlsson, Mats; Hansteen, V. H.; Judge, P. G.; Lites, B. W.; Peter, Hardi; Rosenthal, C. S.; Tarbell, T. D.

doi:10.1086/319103

Cited by 49 publications

(23 citation statements)

References 13 publications

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“…Recently, Judge et al (2001) have detected "magnetic shadows" in time-slice projections from SUMER measurements which they attribute to mode conversion in canopy fibrils (cf. McIntosh et al 2001). In contrast to the power aureoles, these shadows are nearnetwork areas that lack both in brightness and oscillatory power.…”

Section: Spatial Modulation Variationsmentioning

confidence: 95%

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Dynamics of the solar chromosphere

Krijger¹,

Rutten²,

Lites³

et al. 2001

A&A

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137

173

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Abstract. We analyze oscillations in the solar atmosphere using image sequences from the Transition Region and Coronal Explorer (TRACE) in three ultraviolet passbands which sample the upper solar photosphere and low chromosphere. We exploit the absence of atmospheric seeing in TRACE data to furnish comprehensive Fourier diagnostics (amplitude maps, phase-difference spectra, spatio-temporal decomposition) for quiet-Sun network and internetwork areas with excellent sampling statistics. Comparison displays from the ground-based Ca ii H spectrometry that was numerically reproduced by Carlsson & Stein are added to link our results to the acoustic shock dynamics in this simulation. The TRACE image sequences confirm the dichotomy in oscillatory behaviour between network and internetwork and show upward propagation above the cutoff frequency, the onset of acoustic shock formation in the upper photosphere, phase-difference contrast between pseudo-mode ridges and the interridge background, enhanced three-minute modulation aureoles around network patches, a persistent low-intensity background pattern largely made up of internal gravity waves, ubiquitous magnetic flashers, and low-lying magnetic canopies with much low-frequency modulation. The spatio-temporal occurrence pattern of internetwork grains is found to be dominated by acoustic and gravity wave interference. We find no sign of the high-frequency sound waves that have been proposed to heat the quiet chromosphere, but such measurement is hampered by non-simultaneous imaging in different passbands. We also find no signature of particular low-frequency fluxtube waves that have been proposed to heat the network. However, internal gravity waves may play a role in their excitation.

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Section: Spatial Modulation Variationsmentioning

confidence: 95%

“…Again, it is not clear a priori whether this is the case. Magnetic mode conversion seems better established at larger atmospheric height than sampled by the TRACE ultraviolet passbands (McIntosh et al 2001). …”

Section: Spatial Modulation Variationsmentioning

confidence: 99%

Dynamics of the solar chromosphere

Krijger¹,

Rutten²,

Lites³

et al. 2001

A&A

Self Cite

137

173

View full text Add to dashboard Cite

show abstract

“…In practice, this double integral is too computationally expensive to compute, and various approximations are made. The integral over frequency is replaced by four representative radiation bins, with their own associated bin-averaged opacity per mass unit κ i , photon destruction probability i and thermal emission E i , assuming isotropic scattering and isotropic source function and opacity (Nordlund 1982;Skartlien 2000). The radiative heating of such a so-called multi-group scheme is then given by…”

Section: Equation Of State Conservation Of Internal Energy Is Expresmentioning

confidence: 99%

On the minimum temperature of the quiet solar chromosphere

Leenaarts

Carlsson

Hansteen

et al. 2011

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Aims. We aim to provide an estimate of the minimum temperature of the quiet solar chromosphere. Methods. We perform a 2D radiation-MHD simulation spanning the upper convection zone to the lower corona. The simulation includes non-LTE radiative transfer and an equation-of-state that includes non-equilibrium ionization of hydrogen and non-equilibrium H 2 molecule formation. We analyze the reliability of the various assumptions made in our model in order to assess the realism of the simulation. Results. Our simulation contains pockets of cool gas with down to 1660 K from 1 Mm up to 3.2 Mm height. It overestimates the radiative heating, and contains non-physical heating below 1660 K. Therefore we conclude that cool pockets in the quiet solar chromosphere might have even lower temperatures than in the simulation, provided that there exist areas in the chromosphere without significant magnetic heating. We suggest off-limb molecular spectroscopy to look for such cool pockets and 3D simulations including a local dynamo and a magnetic carpet to investigate Joule heating in the quiet chromosphere.

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“…One minor tick corresponds to 5 arcsec. a major role in the higher atmosphere where plasma β (ratio of gas pressure over magnetic pressure) becomes small (McIntosh et al 2001) and wave reflection and conversion between acoustic and magneto-acoustic modes takes place (Rosenthal et al 2002;Bogdan et al 2003).…”

Section: Introductionmentioning

confidence: 99%

On the fine structure of the quiet solar Ca II K atmosphere

Tritschler

Schmidt

Uitenbroek³

et al. 2006

A&A

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Aims. We investigate the morphological, dynamical, and evolutionary properties of the internetwork and network fine structure of the quiet sun at disk centre.Methods. The analysis is based on a ∼6 h time sequence of narrow-band filtergrams centred on the inner-wing Ca ii K 2v reversal at 393.3 nm. To examine the temporal evolution of network and internetwork areas separately we employ a double-Gaussian decomposition of the mean intensity distribution. An autocorrelation analysis is performed to determine the respective characteristic time scales. In order to analyse statistical properties of the fine structure we apply image segmentation techniques. Results. The results for the internetwork are related to predictions derived from numerical simulations of the quiet sun. The average evolutionary time scale of the internetwork in our observations is 52 s. Internetwork grains show a tendency to appear on a mesh-like pattern with a mean cell size of ∼4-5 arcsec. Based on this size and the spatial organisation of the mesh we speculate that this pattern is related to the existence of photospheric downdrafts as predicted by convection simulations. The image segmentation shows that typical sizes of both network and internetwork grains are in the order of 1.6 arcsec.

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An Observational Manifestation of Magnetoatmospheric Waves in Internetwork Regions of the Chromosphere and Transition Region

Cited by 49 publications

References 13 publications

Dynamics of the solar chromosphere

Dynamics of the solar chromosphere

On the minimum temperature of the quiet solar chromosphere

On the fine structure of the quiet solar Ca II K atmosphere

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