Three-minute wave enhancement in the solar photosphere

Stangalini, M.; Giannattasio, Fabio; Moro, D. Del; Berrilli, F.

doi:10.1051/0004-6361/201118654

Cited by 34 publications

(39 citation statements)

References 28 publications

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“…The acoustic emission in both umbral cores peaks around 5−7 mHz, that is, the band of threeminute oscillations. This agrees with Stangalini et al (2012), who showed that the three-minute enhancement is strictly confined to the umbral region, while five-minute waves are suppressed here. Around 4 mHz, the power is dominant in the LB, a plage eastward of the pore, and at the edges of umbral cores.…”

Section: Observed Oscillation Propertiessupporting

confidence: 93%

Dynamics of the solar atmosphere above a pore with a light bridge

Sobotka

Švanda

Jurčák

et al. 2013

A&A

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Context. Solar pores are small sunspots lacking a penumbra that have a prevailing vertical magnetic-field component. They can include light bridges at places with locally reduced magnetic field. Like sunspots, they exhibit a wide range of oscillatory phenomena. Aims. A large isolated pore with a light bridge (NOAA 11005) is studied to obtain characteristics of a chromospheric filamentary structure around the pore, to analyse oscillations and waves in and around the pore, and to understand the structure and brightness of the light bridge. Methods. Spectral imaging observations in the line Ca II 854.2 nm and complementary spectropolarimetry in Fe I lines, obtained with the DST/IBIS spectrometer and HINODE/SOT spectropolarimeter, were used to measure photospheric and chromospheric velocity fields, oscillations, waves, the magnetic field in the photosphere, and acoustic energy flux and radiative losses in the chromosphere. Results. The chromospheric filamentary structure around the pore has all important characteristics of a superpenumbra: it shows an inverse Evershed effect and running waves, and has a similar morphology and oscillation character. The granular structure of the light bridge in the upper photosphere can be explained by radiative heating. Acoustic waves leaking up from the photosphere along the inclined magnetic field in the light bridge transfer enough energy flux to balance the entire radiative losses of the light-bridge chromosphere. Conclusions. A penumbra is not a necessary condition for the formation of a superpenumbra. The light bridge is heated by radiation in the photosphere and by acoustic waves in the chromosphere.

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Section: Observed Oscillation Propertiessupporting

confidence: 93%

Dynamics of the solar atmosphere above a pore with a light bridge

Sobotka

Švanda

Jurčák

et al. 2013

A&A

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“…This is however, insufficient to explain the observed amplification of the threeminute oscillations (Stangalini et al 2012).…”

Section: Introductionmentioning

confidence: 90%

“…Observational results show that the amplitude of the three minute oscillation is not explained well enough by the excitation of the cut-off frequency (Stangalini et al 2012). Furthermore, many observations show a harmonic wave structure (Yuan et al 2011;Reznikova et al 2012;Sych et al 2011) as opposed to the saw-tooth signal required for the shock wave model.…”

Section: Introductionmentioning

confidence: 98%

Chromospheric seismology above sunspot umbrae

Snow

Botha

Régnier

2015

A&A

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Context. The acoustic resonator is an important model for explaining the three-minute oscillations in the chromosphere above sunspot umbrae. The steep temperature gradients at the photosphere and transition region provide the cavity for the acoustic resonator, which allows waves to be both partially transmitted and partially reflected. Aims. In this paper, a new method of estimating the size and temperature profile of the chromospheric cavity above a sunspot umbra is developed. Methods. The magnetic field above umbrae is modelled numerically in 1.5D with slow magnetoacoustic wave trains travelling along magnetic fieldlines. Resonances are driven by applying the random noise of three different colours-white, pink and brown-as small velocity perturbations to the upper convection zone. Energy escapes the resonating cavity and generates wave trains moving into the corona. Line of sight (LOS) integration is also performed to determine the observable spectra through SDO/AIA. Results. The numerical results show that the gradient of the coronal spectra is directly correlated with the chromosperic temperature configuration. As the chromospheric cavity size increases, the spectral gradient becomes shallower. When LOS integrations is performed, the resulting spectra demonstrate a broadband of excited frequencies that is correlated with the chromospheric cavity size. The broadband of excited frequencies becomes narrower as the chromospheric cavity size increases. Conclusions. These two results provide a potentially useful diagnostic for the chromospheric temperature profile by considering coronal velocity oscillations.

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“…This atmospheric region still presents crucial observational and theoretical challenges. In the chromosphere, compressible waves excited at the photospheric roots of the granular convection, or through p-mode conversion, steepen and form shocks, accounting for large dynamical excursions and very short timescales, of a few minutes at most, [14][15][16] requiring a fully time-dependent analysis. Understanding the mechanisms that sustain the chromosphere departure from radiative equilibrium will pave the way to understanding the formation of the super-hot corona and the origin of the solar wind.…”

Section: Chromosphere Fast Dynamicsmentioning

confidence: 99%

“…Among the many different kinds of MHD waves that small flux tubes can support (compressive and noncompressive), kink waves are probably the most promising due to their ability to travel long distances before being dissipated. 15,16,25,26 Very recently, observations have revealed the propagation of kink waves in small magnetic elements to the solar chromosphere, with velocity of the order of 6 km∕s. 27 However, although these authors have shown that this propagation is highly nonlinear, and thus subject to dissipation, no signature of energy losses was found between the photosphere and the chromosphere.…”

Section: Waves and Heating Of The Solar Upper Atmospherementioning

confidence: 99%

ADAHELI+: exploring the fast, dynamic Sun in the x-ray, optical, and near-infrared

Berrilli

Soffitta

Velli

et al. 2015

J. Astron. Telesc. Instrum. Syst

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Abstract. Advanced Astronomy for Heliophysics Plus (ADAHELI+) is a project concept for a small solar and space weather mission with a budget compatible with an European Space Agency (ESA) S-class mission, including launch, and a fast development cycle. ADAHELI+ was submitted to the European Space Agency by a European-wide consortium of solar physics research institutes in response to the "Call for a small mission opportunity for a launch in 2017," of March 9, 2012. The ADAHELI+ project builds on the heritage of the former ADAHELI mission, which had successfully completed its phase-A study under the Italian Space Agency 2007 Small Mission Programme, thus proving the soundness and feasibility of its innovative low-budget design. ADAHELI+ is a solar space mission with two main instruments: ISODY+: an imager, based on Fabry-Pérot interferometers, whose design is optimized to the acquisition of highest cadence, long-duration, multiline spectropolarimetric images in the visible/near-infrared region of the solar spectrum. XSPO: an x-ray polarimeter for solar flares in x-rays with energies in the 15 to 35 keV range. ADAHELI+ is capable of performing observations that cannot be addressed by other currently planned solar space missions, due to their limited telemetry, or by ground-based facilities, due to the problematic effect of the terrestrial atmosphere. © The Authors. Published by SPIE under a Creative Commons Attribution 3.0 Unported License. Distribution or reproduction of this work in whole or in part requires full attribution of the original publication, including its DOI.

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Three-minute wave enhancement in the solar photosphere

Cited by 34 publications

References 28 publications

Dynamics of the solar atmosphere above a pore with a light bridge

Dynamics of the solar atmosphere above a pore with a light bridge

Chromospheric seismology above sunspot umbrae

ADAHELI+: exploring the fast, dynamic Sun in the x-ray, optical, and near-infrared

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