A Study of Solar Prominences near lambda = 1 Millimeter

Bastian, T. S.; Ewell, M. W.; Zirin, H.

doi:10.1086/173413

Cited by 28 publications

(30 citation statements)

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“…Here we follow a similar approach to that of Bastian, Ewell, and Zirin (1993). In the fourth observational cycle of ALMA, the two wavelength bands available to solar physicists are Band 6 (1.3 mm) and Band 3 (3.0 mm).…”

Section: Plasma Diagnosticsmentioning

confidence: 99%

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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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Section: Plasma Diagnosticsmentioning

confidence: 99%

“…Vrsnak et al, 1992;Bastian, Ewell, and Zirin, 1993;Harrison et al, 1993;Irimajiri et al, 1995). Studies of prominences and filaments at centimeter wavelengths have also been conducted (see e.g.…”

Section: Introductionmentioning

confidence: 99%

Solar Prominence Modelling and Plasma Diagnostics at ALMA Wavelengths

Rodger

Labrosse

2017

Sol Phys

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“…The first SMM observations of an active prominence have been performed by Harrison et al (1993). Bastian et al (1993) later studied several prominences and filaments using observations at two different SMM wavelengths. A further study was performed by Irimajiri et al (1995) using observations at three different SMM wavelengths.…”

Section: Introductionmentioning

confidence: 99%

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

Gunár

Heinzel

Mackay

et al. 2016

ApJ

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We use the detailed 3D whole-prominence fine structure model to produce the first simulated high-resolution ALMA observations of a modeled quiescent solar prominence. The synthetic brightness temperature and optical thickness maps shown in the present paper are produced using a visualization method for the sub-millimeter/millimeter radio continua synthesis. We have obtained the simulated observations of both the prominence at the limb and the filament on the disk at wavelengths covering a broad range which encompasses the full potential of ALMA. We demonstrate here to what extent the small-scale and large-scale prominence and filament structures will be visible in the ALMA observations spanning both the optically thin and thick regimes. We analyze the relationship between the brightness and kinetic temperature of the prominence plasma. We also illustrate the opportunities ALMA will provide for studying the thermal structure of the prominence plasma from the cool prominence fine structure cores to the prominence-corona transition region. In addition, we show that the detailed 3D modeling of entire prominences with their numerous fine structures will be important for the correct interpretation of future ALMA prominence observations.

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“…Bommier et al (1986Bommier et al ( , 1994 found n e in the range 3 xlO 9 -4 x 10 10 cm" 3 ). Radio prominence measurements performed in the mm range with the VLA (Bastian et al 1993) and the JCMT (Harrison et al 1993) also point to low values (about 10 10 cm -3 ). Of course, the very existence of such low densities implies large effective thicknesses, as noted by Hirayama (1990).…”

Section: Densitiesmentioning

confidence: 97%

Solar Prominence Diagnostics

Vial

1998

International Astronomical Union Colloquium

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Abstract. This paper reviews the diagnostic techniques currently used to establish estimates of the physical properties of prominences. Most often the fine structure of prominences cannot be resolved. Because of this and the complex structures and the varied forms of prominences, it is difficult to establish definitive values for temperature, density, magnetic field, electric field, differential emission measure, mass flows, etc. Nevertheless, there are many useful techniques ranging from spectroscopic analysis to measurements of prominence oscillations. Most of the major techniques are reviewed in this paper, with examples of the results and an extensive bibliography. Special attention is paid to the potential diagnostic value of optically thick lines. Suggestions are made for further progress based on SOHO and other observations.

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A Study of Solar Prominences near lambda = 1 Millimeter

Cited by 28 publications

References 0 publications

Solar Prominence Modelling and Plasma Diagnostics at ALMA Wavelengths

Solar Prominence Modelling and Plasma Diagnostics at ALMA Wavelengths

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

Solar Prominence Diagnostics

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