Simultaneous multifrequency observations of an eruptive prominence at millimeter wavelengths

Irimajiri, Yoshihisa; Takano, Toshiaki; Nakajima, Hiroshi; Shibasaki, Κ.; Hanaoka, Yoichiro; Ichimoto, Kiyoshi

doi:10.1007/bf00670232

Cited by 30 publications

(25 citation statements)

References 18 publications

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“…see also Irimajiri et al (1995); Gopalswamy et al (1998), or Loukitcheva et al (2004. In the present paper we take the same α = 0.018 g ff as in Heinzel et al (2015a) -for more details see the discussion therein -and we also assume g ff = 1.…”

Section: Synthesis Of Smm Radio Continuamentioning

confidence: 99%

“…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. However, such single dish aperture observations provide only limited spatial resolution and thus cannot be used to determine the thermal properties of the prominence fine structures.…”

Section: Introductionmentioning

confidence: 99%

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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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Section: Synthesis Of Smm Radio Continuamentioning

confidence: 99%

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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“…observations at 0.85 mm reported by Bastian et al 1993 andLindsey et al 1995 had a resolution of ∼20 ) or by using larger telescopes (e.g. the Nobeyama 45-m telescope which yields a resolution of ∼20 at λ = 3 mm; see Irimajiri et al 1995). Furthermore, during solar eclipses, the edge of the Moon has been used to gain high resolution in one dimension (e.g.…”

Section: Introductionmentioning

confidence: 99%

Center-to-limb observations of the Sun with ALMA

Alissandrakis

Patsourakos

Nindos

et al. 2017

A&A

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Aims. To derive information on the temperature structure of the solar chromosphere and compare it with existing models. Methods. We measured the center-to-limb variation of the brightness temperature, T b , from ALMA full-disk images at two frequencies and inverted the solution of the transfer equation to obtain the electron temperature, T e as a function of optical depth, τ. Results. The ALMA images are very similar to AIA images at 1600 Å. The brightness temperature at the center of the disk is 6180 and 7250 K at 239 and 100 GHz respectively, with dispersions of 100 and 170 K. Plage regions stand out clearly in the 239/100 GHz intensity ratio, while faculae and filament lanes do not. The solar disk radius, reduced to 1 AU, is 961.1 ± 2.5 and 964.1 ± 4.5 at 239 and 100 GHz respectively. A slight but statistically significant limb brightening is observed at both frequencies. Conclusions. The inversion of the center-to-limb curves shows that T e varies linearly with the logarithm of optical depth for 0.34 < τ 100 GHz < 12, with a slope d ln T e /dτ = −608 K. Our results are 5% lower than predicted by the average quiet sun model C of Fontenla et al. (1993), but do not confirm previous reports that the mm-λ solar spectrum is better fitted with models of the cell interior.

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“…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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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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Simultaneous multifrequency observations of an eruptive prominence at millimeter wavelengths

Cited by 30 publications

References 18 publications

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

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

Center-to-limb observations of the Sun with ALMA

Solar Prominence Modelling and Plasma Diagnostics at ALMA Wavelengths

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