Quiescent Prominences in the Era of Alma: Simulated Observations Using the 3d Whole-Prominence Fine Structure Model

Gunár, S.; Heinzel, P.; Mackay, D. H.; Anzer, U.

doi:10.3847/1538-4357/833/2/141

Cited by 15 publications

(18 citation statements)

References 32 publications

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“…19b; Gunár et al. 2016). This is an intrinsically static approach; however, the time evolution of fine structures was also obtained in the form of a sequence of quasistatic equilibria by allowing the photospheric magnetic boundary to change, and with it the 3D NLFF magnetic skeleton (Gunár and Mackay 2015b).…”

Section: Adding Flesh and Blood To The Skeleton: Incorporating Dynamimentioning

confidence: 98%

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Solar prominences: theory and models

Gibson

2018

Living Rev Sol Phys

118

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Magnetic fields suspend the relatively cool material of solar prominences in an otherwise hot corona. A comprehensive understanding of solar prominences ultimately requires complex and dynamic models, constrained and validated by observations spanning the solar atmosphere. We obtain the core of this understanding from observations that give us information about the structure of the “magnetic skeleton” that supports and surrounds the prominence. Energetically-sophisticated magnetohydrodynamic simulations then add flesh and blood to the skeleton, demonstrating how a thermally varying plasma may pulse through to form the prominence, and how the plasma and magnetic fields dynamically interact.

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Section: Adding Flesh and Blood To The Skeleton: Incorporating Dynamimentioning

confidence: 98%

“…b Prominence fine structure in (top) H emission and (bottom) 9.0 mm (33 GHz) brightness temperature determined from plasma in 1D hydrostatic equilibrium along field lines within a 3D NLFF magnetic model (from Gunár et al. 2016). Images reproduced with permission, copyright by AAS…”

Section: Adding Flesh and Blood To The Skeleton: Incorporating Dynamimentioning

confidence: 99%

Solar prominences: theory and models

Gibson

2018

Living Rev Sol Phys

118

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“…The visualisation of how whole prominences may look when observed with ALMA has been simulated by Heinzel et al (2015a) and Gunár et al (2016). The former used a method to convert a calibrated Hα intensity map into an estimated brightness temperature observation.…”

Section: Discussionmentioning

confidence: 99%

“…Simulated observations of whole prominences in the mm domain have been created by Gunár et al (2016) using a 3D whole-prominence fine-structure model. The prominence fine structures are formed within dips in a synthetic prominence magnetic field.…”

Section: Introductionmentioning

confidence: 99%

Solar Prominence Modelling and Plasma Diagnostics at ALMA Wavelengths

Rodger

Labrosse

2017

Sol Phys

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Our aim is to test potential solar prominence plasma diagnostics as obtained with the new solar capability of the Atacama Large Millimeter/submillimeter Array (ALMA). We investigate the thermal and plasma diagnostic potential of ALMA for solar prominences through the computation of brightness temperatures at ALMA wavelengths. The brightness temperature, for a chosen line of sight, is calculated using the densities of electrons, hydrogen, and helium obtained from a radiative transfer code under non-local thermodynamic equilibrium (non-LTE) conditions, as well as the input internal parameters of the prominence model in consideration. Two distinct sets of prominence models were used: isothermal-isobaric fine-structure threads, and large-scale structures with radially increasing temperature distributions representing the prominence-to-corona transition region. We compute brightness temperatures over the range of wavelengths in which ALMA is capable of observing (0.32 -9.6 mm), however, we particularly focus on the bands available to solar observers in ALMA cycles 4 and 5, namely 2.6 -3.6 mm (Band 3) and 1.1 -1.4 mm (Band 6). We show how the computed brightness temperatures and optical thicknesses in our models vary with the plasma parameters (temperature and pressure) and the wavelength of observation. We then study how ALMA observables such as the ratio of brightness temperatures at two frequencies can be used to estimate the optical thickness and the emission measure for isothermal and non-isothermal prominences. From this study we conclude that for both sets of models, ALMA presents a strong thermal diagnostic capability, provided that the interpretation of observations is supported by the use of non-LTE simulation results.

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“…But as discussed above, the finestructure dynamics is not affecting our results based on continuum observations, only some marginal influence can be expected on integrated Hα emission. Fully 3D modeling of ALMA visibility of heterogeneous prominences was already performed in Gunár et al (2016) and Gunár et al (2018), but the next step is to consider relevant inversion strategies. The principal conclusion here is that ALMA provides reliable data for prominence temperature diagnostics and these data give the results which are consistent with the Hα observations.…”

Section: Discussion and Future Prospectsmentioning

confidence: 99%

ALMA as a prominence thermometer: First observations

Heinzel,

Berlicki,

Bárta

et al. 2022

Preprint

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We present first prominence observations obtained with ALMA in Band 3 at the wavelength of 3 mm. High-resolution observations have been coaligned with the MSDP Hα data from Wroc law-Bia lków large coronagraph at similar spatial resolution. We analyze one particular co-temporal snapshot, first calibrating both ALMA and MSDP data and then demonstrating a reasonable correlation between both. In particular we can see quite similar fine-structure patterns in both ALMA brightness temperature maps and MSDP maps of Hα intensities. Using ALMA we intend to derive the prominence kinetic temperatures. However, having current observations only in one band, we use an independent diagnostic constraint which is the Hα line integrated intensity. We develop an inversion code and show that it can provide realistic temperatures for brighter parts of the prominence where one gets a unique solution, while within faint structures such inversion is ill conditioned. In brighter parts ALMA serves as a prominence thermometer, provided that the optical thickness in Band 3 is large enough. In order to find a relation between brightness and kinetic temperatures for a given observed Hα intensity, we constructed an extended grid of non-LTE prominence models covering a broad range of prominence parameters. We also show the effect of the plane-of-sky filling factor on our results.

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Quiescent Prominences in the Era of Alma: Simulated Observations Using the 3d Whole-Prominence Fine Structure Model

Cited by 15 publications

References 32 publications

Solar prominences: theory and models

Solar prominences: theory and models

Solar Prominence Modelling and Plasma Diagnostics at ALMA Wavelengths

ALMA as a prominence thermometer: First observations

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