4.4 Review

Waves in the lower solar atmosphere: the dawn of next-generation solar telescopes

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DeSIRe: Departure coefficient aided Stokes Inversion based on Response functions

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Summary: This article introduces a new inversion code called DeSIRe, which integrates the well-known inversion code SIR with the NLTE radiative transfer solver RH. It aims to solve the non-local thermodynamic equilibrium (NLTE) problem in observing chromospheric spectral lines. The code is characterized by its fast runtime, robustness, stability, and has been made publicly available for use in the solar community.

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Large scale coherent magnetohydrodynamic oscillations in a sunspot

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Summary: This study reports the observation of the largest-scale coherent oscillations in a sunspot, with a spectrum different from the Sun's global acoustic oscillations, incorporating a superposition of many resonant wave modes.

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Magnetohydrodynamic Wave Mode Identification in Circular and Elliptical Sunspot Umbrae: Evidence for High-order Modes

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Summary: This study provides clear direct evidence of multiple concurrent higher-order magnetohydrodynamic (MHD) modes in circular and elliptical sunspots using proper orthogonal decomposition (POD) and dynamic mode decomposition (DMD) techniques on solar observational data. The analysis showed the presence of fundamental and higher-order MHD wave modes in both types of sunspots, highlighting the importance of ellipticity and irregularities in umbral cross-sectional shapes for accurate modeling.

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High-frequency Waves in Chromospheric Spicules

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Summary: In this study, we investigated the statistical properties of transverse oscillations in spicules using high-cadence observations. We found that the oscillations exhibit different displacement and velocity amplitudes at different heights, and there are various types of oscillations including upward propagating, downward propagating, and standing waves. Additionally, we observed a decrease in energy flux as the oscillations propagate upwards.

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The European Solar Telescope

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Summary: The European Solar Telescope is a project aimed at studying the magnetic connectivity of the solar atmosphere, and it will become the most powerful European ground-based facility to study the Sun in the coming decades, using the most innovative technological advances.

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Propagation of transverse waves in the solar chromosphere probed at different heights with ALMA sub-bands

Juan Camilo Guevara Gomez et al.

Summary: ALMA has provided an excellent diagnostic tool for studying the dynamics of the Solar chromosphere, with observations limited to full-band data products. By analyzing ALMA Band 3 data, a dynamic event involving wave propagation was observed, revealing statistical results on propagation speed and energy flux.

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The Propagation of Coherent Waves Across Multiple Solar Magnetic Pores

S. D. T. Grant et al.

Summary: Solar pores act as efficient magnetic conduits to propagate magnetohydrodynamic wave energy into the outer solar atmosphere. Wave activity within different regions of the solar atmosphere, from photosphere to chromosphere, showed complex patterns and behavior, with wave coherence diminishing as they propagate into the chromosphere. Despite introducing equivalent wave modes into similar pores in the photosphere, vast differences in wave morphology at chromospheric layers were observed.

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Ambipolar Diffusion in the Lower Solar Atmosphere: Magnetohydrodynamic Simulations of a Sunspot

Conor D. MacBride et al.

Summary: Magnetohydrodynamic (MHD) simulations assume fully ionized plasma, but in the lower solar atmosphere, reduced temperature leads to partial ionization. The interaction between neutral and ionized components produces ambipolar diffusion. Studying the propagation of magnetoacoustic waves above sunspot umbra, we find that ambipolar diffusion plays a pivotal role in wave characteristics in weakly ionized low density regions. It is important to consider ambipolar diffusion in simulations and interpretation of solar observations.

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Reply to: Signatures of sunspot oscillations and the case for chromospheric resonances

David B. Jess et al.

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Signatures of sunspot oscillations and the case for chromospheric resonances

Tobias Felipe

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Vortex flow properties in simulations of solar plage region: Evidence for their role in chromospheric heating

N. Yadav et al.

Summary: This study investigates the physical properties of small-scale vortices inside magnetic flux tubes in the solar atmosphere and explores their potential role in heating the solar chromosphere. Small-scale vortices were found to be denser and hotter structures that contribute to chromospheric heating by dissipating current sheets formed at their interfaces.

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Downflowing umbral flashes as evidence of standing waves in sunspot umbrae

T. Felipe et al.

Summary: Recent studies have reported umbral flashes in downflowing atmospheres, indicating a shift from previous associations with upflows. The presence of standing oscillations above sunspot umbrae has been found to explain the phenomena of downflowing umbral flashes.

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Combining magneto-hydrostatic constraints with Stokes profiles inversions: II. Application to Hinode/SP observations

J. M. Borrero et al.

Summary: In this study, a new inversion code is developed to reliably infer the physical parameters in the (x, y, z) domain by combining an inverse solver for the radiative transfer equation with a solver for the magneto-hydrostatic equilibrium. The new code is tested with spectropolarimetric observations of sunspots recorded with the Hinode spacecraft, showing improvements in determining physical parameters and the Wilson depression of sunspots in three dimensions. This approach opens up the possibility of calculating reliable electric currents in the solar photosphere and warrants further comparisons with alternative methods.

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Acoustic-gravity wave propagation characteristics in three-dimensional radiation hydrodynamic simulations of the solar atmosphere

B. Fleck et al.

Summary: In the past decades, there has been tremendous progress in the degree of realism of three-dimensional radiation magneto-hydrodynamic simulations of the solar atmosphere. The study found considerable differences between the various models in terms of wave propagation characteristics, with the height dependence of wave power, especially high-frequency waves, varying significantly. The phase difference spectra of several models showed unexpected features, including 180 degrees phase jumps.

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Oscillations observed in umbra, plage, quiet-Sun and the polarity inversion line of active region 11158 using Helioseismic Magnetic Imager/Solar Dynamics Observatory data

A. A. Norton et al.

Summary: This study used data from the Helioseismic Magnetic Imager to investigate the oscillations in quiet-Sun, plage, umbra, and an active region, revealing phase relations through Fourier, wavelet, and cross-correlation analysis. Different line width variations and phase relations were observed in different regions, offering a potential way to differentiate wave mode mechanics effectively. The presence of significant Doppler velocity oscillations along the PIL suggests the presence of Alvenic waves, while time-distance diagrams show the conversion of Eastward propagating Doppler oscillations into magnetic oscillations.

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Characterization of shock wave signatures at millimetre wavelengths from Bifrost simulations

Henrik Eklund et al.

Summary: Observations at millimetre wavelengths are valuable for studying small-scale dynamics in the solar chromosphere, with simulations and measurements showing the characteristics of shock wave propagation and its impact on the atmosphere. The results demonstrate efficient tracking of upwardly propagating shock waves and potential diagnostic tools for understanding small-scale dynamics.

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A new method for detecting solar atmospheric gravity waves

Daniele Calchetti et al.

Summary: The article introduces a new method for studying the propagation of gravity waves in the solar atmosphere by calculating the 3D cross-correlation function of vertical velocities measured at different heights. The authors apply this method to observational data and simulation results, showing preliminary findings and outlining future prospects.

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An overall view of temperature oscillations in the solar chromosphere with ALMA

S. Jafarzadeh et al.

Summary: ALMA has introduced a new diagnostic tool for studying the solar chromosphere through direct measurements of gas temperature. The analysis of multiple datasets reveals varying frequency characteristics in different solar regions and discusses the correlation with magnetic topology, as well as potential reasons for power suppression at around 5.5mHz in ALMA observations.

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High-resolution wave dynamics in the lower solar atmosphere

D. B. Jess et al.

Summary: The Sun's photosphere provides a unique platform for studying, observing, and interpreting waves generated across a wide range of spatial and temporal scales. A focused science team discussed current challenges in wave studies, collaborated to produce 15 independent publications, and explored implications for next-generation observing and computing facilities. This article is part of the Theo Murphy meeting issue 'High-resolution wave dynamics in the lower solar atmosphere'.

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Accurately constraining velocity information from spectral imaging observations using machine learning techniques

Conor D. MacBride et al.

Summary: A novel method using machine learning techniques is presented to identify and isolate the underlying components present in observed spectral lines, constraining their profiles through Voigt fits. The study validates the code's suitability for extracting two-component atmospheric profiles in sunspot chromospheres, achieving reliable results with median reduced chi (2) values equal to 1.03.

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Proper orthogonal and dynamic mode decomposition of sunspot data

A. B. Albidah et al.

Summary: The study demonstrates the successful identification of sausage and kink modes in a sunspot umbra using a combination of POD and DMD techniques, providing new insights into solar observations.

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The dynamics of 3-min wavefronts and their relation to sunspot magnetic fields

Robert Sych et al.

Summary: This study conducted spectral analysis of wave processes occurring in a solar active region on December 10, 2010, revealing that wave trains moved along a preferential direction and could be represented as separate narrowband oscillation sources. The observed spirality of wavefronts and activation of umbral structures were associated with the motion path of the waves and temporal dynamics of the sources.

PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY A-MATHEMATICAL PHYSICAL AND ENGINEERING SCIENCES (2021)

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Transverse motions in sunspot super-penumbral fibrils

R. J. Morton et al.

Summary: Sunspots are crucial in understanding magnetohydrodynamic (MHD) wave phenomena in the Sun's atmosphere, with recent studies revealing the presence of transverse wave modes in the majority of the chromosphere. High-resolution observations show transverse motions in chromospheric super-penumbral fibrils, interpreted as MHD kink modes. Statistical properties of over 2000 transverse motions are consistent with previous observations, raising important questions about wave generation and energy transfer in sunspot atmospheres.

PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY A-MATHEMATICAL PHYSICAL AND ENGINEERING SCIENCES (2021)

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On the effect of oscillatory phenomena on Stokes inversion results

P. H. Keys et al.

Summary: This study investigates the impact of propagating MHD waves in flux tubes on the inversion of solar atmospheric parameters using simulated data and Stokes inversion methods. The results show that the inverted atmospheric parameters match well with the simulated data and have higher accuracy at typical formation heights.

PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY A-MATHEMATICAL PHYSICAL AND ENGINEERING SCIENCES (2021)

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On the influence of magnetic topology on the propagation of internal gravity waves in the solar atmosphere

G. Vigeesh et al.

Summary: This study simulates the propagation of internal gravity waves in the solar atmosphere under different magnetic field topologies. It is found that in models with predominantly horizontal magnetic fields, gravity waves propagate upwards, while in models with predominantly vertical magnetic fields, the waves propagate downwards. This reveals a crucial difference in the propagation direction of gravity waves in the solar atmosphere.

PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY A-MATHEMATICAL PHYSICAL AND ENGINEERING SCIENCES (2021)

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High-frequency oscillations in small chromospheric bright features observed with Atacama Large Millimetre/Submillimetre Array

J. C. Guevara Gomez et al.

Summary: Detection of oscillations in brightness temperature, size and horizontal velocity of small bright features in the chromosphere suggests the presence of fast sausage-mode waves and possibly Alfvenic oscillations. These high-frequency magnetohydrodynamic waves may channel energy into the outer atmosphere of the Sun.

PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY A-MATHEMATICAL PHYSICAL AND ENGINEERING SCIENCES (2021)

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Magnetoacoustic wave energy dissipation in the atmosphere of solar pores

Caitlin A. Gilchrist-Millar et al.

Summary: Observational evidence of magnetohydrodynamic wave activity in solar pores is presented, with energy fluxes decreasing at higher atmospheric heights, suggesting solar pores can efficiently guide wave energy upwards. The study highlights the presence of both body- and surface-mode sausage waves in solar pores.

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Influence of ambipolar and Hall effects on vorticity in three-dimensional simulations of magneto-convection

E. Khomenko et al.

Summary: This paper presents the results of three-dimensional simulations of solar magneto-convection with the joint action of ambipolar diffusion and the Hall effect. The ambipolar diffusion reduces vorticity and converts it into thermal energy, while the Hall effect enhances vorticity and produces more vertical magnetic field structures.

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Spectropolarimetric fluctuations in a sunspot chromosphere

M. Stangalini et al.

Summary: The instrumental advances in 4m class solar telescopes allow for unprecedented detail in studying chromospheric magnetic fields and MHD wave processes. Recent research using cutting-edge spectropolarimetric observations has revealed a clear link between intensity and circular polarization fluctuations in a specific area of a sunspot chromosphere, suggesting the presence of Alfvenic perturbations.

PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY A-MATHEMATICAL PHYSICAL AND ENGINEERING SCIENCES (2021)

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IRIS observations of chromospheric heating by acoustic waves in solar quiet and active regions

V Abbasvand et al.

Summary: The study found that acoustic and magnetoacoustic waves play a significant role in heating the chromosphere, with acoustic waves compensating for a substantial fraction of radiative losses in quiet regions. However, in active regions, their contribution is too small to balance the radiative losses and other heating mechanisms are involved.

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Finding the mechanism of wave energy flux damping in solar pores using numerical simulations

J. M. Riedl et al.

Summary: The study investigates the damping mechanisms of energy flux in solar magnetic pores using numerical simulations and observations. It reveals that the strong damping observed in the energy flux is mainly caused by geometric spreading due to diverging field lines and lateral wave leakage. Ideal and non-ideal MHD simulations with a plane driver cannot reproduce the observed damping, while simulations with a localized driver closely correspond with the observations.

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Temporal evolution of small-scale internetwork magnetic fields in the solar photosphere

R. J. Campbell et al.

Summary: The study reveals the presence of ubiquitous small-scale transverse magnetic fields in the quiet Sun internetwork region, which exhibit complex structures. High-resolution observations and magnetic inversion techniques can be used to characterize and track the dynamic evolution of these small-scale magnetic features.

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Computing Helioseismic Sensitivity Kernels for the Sun's Large-scale Internal Flows Using Global-scale Wave-propagation Simulations

Thomas Hartlep et al.

Summary: Helioseismic waves on the solar surface can be used to probe the interior properties of the Sun, such as flows. A new method is introduced to derive three-dimensional sensitivity kernels for large-scale horizontal flows in the solar interior, showing that transverse components are important in inversions for interior flows. Global-Sun wave-propagation simulations are used to measure the shifts in helioseismic travel times caused by flow perturbations.

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A novel approach to identify resonant MHD wave modes in solar pores and sunspot umbrae: B - ω analysis

M. Stangalini et al.

Summary: The study explores an unusual oscillation phenomenon in pores of sunspots, where a dominant frequency of 5 mHz is observed instead of the expected 3 mHz. By analyzing Doppler velocities and spectropolarimetry, researchers have identified distinct ridges in the B-omega diagram that are clear signatures of resonant magneto-hydrodynamic (MHD) oscillations confined within the pore umbra. This novel finding opens up a new avenue for identifying MHD wave modes in the umbral regions of both pores and sunspots.

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Exploring the Sun's upper atmosphere with neural networks: Reversed patterns and the hot wall effect

H. Socas-Navarro et al.

Summary: A inversion procedure based on artificial neural networks was developed for high-resolution solar spectro-polarimeters, which revealed interesting phenomena such as a hot fine-scale network structure and reversed temperature enhancements in the middle and upper photosphere when applied to Hinode data. These findings provide direct observational evidence of the hot wall effect predicted by theoretical models from the 1970's.

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Magnetohydrodynamic Wave Modes of Solar Magnetic Flux Tubes with an Elliptical Cross Section

Anwar A. Aldhafeeri et al.

Summary: This study investigates the behavior of MHD wave modes propagating in compressible magnetic flux tubes with an elliptical cross section, finding that solutions in the form of even Mathieu functions are more sensitive to eccentricity. It also shows that the sausage mode may not be easily identified with increased ellipticity, and that even solutions representing the fluting mode can be misinterpreted as a kink mode. Additionally, kink and sausage surface modes are less affected by ellipticity compared to the fluting modes.

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Critical Science Plan for the Daniel K. Inouye Solar Telescope (DKIST)

Mark P. Rast et al.

Summary: The Daniel K. Inouye Solar Telescope (DKIST) will revolutionize our ability to study the basic physical processes of the Sun and its atmosphere. The Critical Science Plan (CSP) anticipates some of the capabilities enabled by DKIST, focusing on scientific pursuits that are uniquely contributed by DKIST.

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Chromospheric Heating by Magnetohydrodynamic Waves and Instabilities

A. K. Srivastava et al.

Summary: This review focuses on the importance of the chromosphere in mass and energy transport within the solar atmosphere. It discusses the physics of magnetohydrodynamic waves and instabilities in large-scale chromospheric structures and magnetic flux tubes, and also highlights key observational aspects that aid in understanding the role of the solar chromosphere in various dynamic processes and wave phenomena. Additionally, the heating scenario of the solar chromosphere is examined, along with potential implications, future trends, and outstanding questions in this field.

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Identifying Acoustic Wave Sources on the Sun. I. Two-dimensional Waves in a Simulated Photosphere

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