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Reginald, N. L.; Davila, J. M.

doi:10.1023/a:1005251808764

Cited by 26 publications

(13 citation statements)

References 2 publications

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“…The reddening with distance is revealed for the whole corona indicating the red-shifting of the K-corona spectrum due to the outward bulk flow speed of the coronal electrons theoretically predicted by Reginald and Davila [2000] and Reginald et al [2009]. The range < 1.3 R ⊙ is traced by blue features that may be explained by scattering by bound electrons and by the existence of a very small amount of neutral atoms.…”

Section: 1002/2016ja022623mentioning

confidence: 63%

“…The revival of interest to comparisons of the photosphere and K-corona continuum is explained by the possibility of diagnostics of thermal and nonthermal electrons. Cram [1976] suggested spectral technique to determine the electron temperature and flow speed of the coronal electrons, which was significantly extended by Reginald and Davila [2000]. The technique was used by Ichimoto et al [1996].…”

Section: High-precision Measurements Of the Corona Colormentioning

confidence: 99%

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Imaging the structure of the low K‐corona

et al. 2017

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The first 2‐D distributions of the polarization angle and of the relative color index for the K‐corona of 29 March 2006 are presented. The distributions illustrate the efficiency of the total solar eclipse approach for high‐precision measurements of the K‐corona continuum in the range < 1.4 R⊙. Natural ground and space total solar eclipses caused by external occulting the bright solar‐disk light by the Moon or Earth group planets are discussed. Calculations of the eclipse magnitude m are carried out to show ideal conditions for total solar eclipse observations in space from Lagrange point L2 for Mars (m ≈ 1.025). The illumination in Mars' shadow is estimated to equal 5.6 × 10−11 for the wavelength of 550 nm. No internal or external occulting coronagraphs are needed. Partial solar eclipses with m > 0.91 can be observed from Lagrange points L2 for Mercury, Venus, and Earth.

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Section: 1002/2016ja022623mentioning

confidence: 63%

Section: High-precision Measurements Of the Corona Colormentioning

confidence: 99%

Imaging the structure of the low K‐corona

et al. 2017

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“…Через 20 лет Ichimoto et al [1976] экспериментально подтвердили такую возможность, определив T e и V e электронов по результатам наблюдений полного солнечного затмения (ПСЗ) 1994 г. Reginald and Davila [2000] модифицировали подход. Недостатки спектральных методов: получение информации только вдоль направления щели; возможное искажение результатов сравнения непрерывных спектров фотосферы и короны вследствие инструментальной поляризации спектрографа [Липский 1958].…”

Section: Doi: 1031725/0552-5829-2018-211-214unclassified

Continuum Color as an Indicator of Corona Expanding

Kim¹,

Krusanova²,

Попов³

2018

Proceedings of the 22nd All-Russia Conference on Solar and Solar-Terrestrial Physics

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“…By measuring the K-coronal spectrum to an accuracy of 1% we may be able to measure the coronal temperatures and its bulk flow velocity to accuracy within ± 0.2 MK and ± 200 km/sec, respectively. A complete derivation is provided in Reginald (2000). …”

Section: Wavelength In Angstrornsmentioning

confidence: 99%

Coronal electron velocity and temperature from Thomson scattered visible light

Davila

Reginald

Cyr

2005

Solar Physics and Space Weather Instrumentation

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The measurements of velocity and temperature of coronal electrons are of immense importance to the study of coronal dynamics, especially in the low solar corona. In this lies interesting physics yet to fully explain the theoretical reasoning for the million degree hot coronal plasma and the cause for the initial acceleration of this coronal plasma. In this regard it would be equally important if both of these coronal electron parameters, namely the velocity and the temperature of these coronal electrons, could be determined simultaneously and globally all around the low solar corona. The purpose of this paper is twin fold. First, to lay out an instrumental procedure that allows for the measurement of a coronal signature that could measure all around the low solar corona simultaneously. Second, to describe a theoretical procedure that allows for deriving both the coronal electron temperature and its bulk flow velocity from the measured coronal signature.

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Untitled

Cited by 26 publications

References 2 publications

Imaging the structure of the low K‐corona

Imaging the structure of the low K‐corona

Continuum Color as an Indicator of Corona Expanding

Coronal electron velocity and temperature from Thomson scattered visible light

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