The polarization of the solar corona on March 29, 2006

Molodenskii, M. M.; Starkova, L. I.; Kutvitskii, V. A.; Merzlyakov, V. L.

doi:10.1134/s1063772909030093

Cited by 7 publications

(7 citation statements)

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“…Here, we report detailed observations of the combination of coronal polarization and the polarization of the surrounding sky. Such neutral points were predicted by [17], and (hints of them) also observed for earlier solar eclipses [18][19][20][21]. Much in the same fashion as the occurrence of polarization neutral points arXiv:2007.12482v1 [astro-ph.SR] 23 Jul 2020 in the cloud-free sky due to the cancellation of the tangential polarization due to single Rayleigh scattering by the vertical multiple-scattering component, we observe polarization neutral points where the tangential coronal polarization due to Thomson scattering is cancelled by the multiply scattered sky polarization.…”

Section: Introductionmentioning

confidence: 56%

Detection of polarization neutral points in observations of the combined corona and sky during the 21 August 2017 total solar eclipse

et al. 2020

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We report the results of polarimetric observations of the total solar eclipse of Aug. 21 2017 from Rexburg, ID (USA). We use three synchronized DSLR cameras with polarization filters oriented at 0, 60 and 120 degrees to provide high-dynamic-range RGB polarization images of the corona and surrounding sky. We measure tangential coronal polarization and vertical sky polarization, both as expected. These observations provide detailed detections of polarization neutral points above and below the eclipsed Sun where the coronal polarization is cancelled by the sky polarization. We name these special polarization neutral points after Minnaert and Van de Hulst.

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Section: Introductionmentioning

confidence: 56%

Detection of polarization neutral points in observations of the combined corona and sky during the 21 August 2017 total solar eclipse

et al. 2020

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“…This difference is apparently caused by the insufficient quality of our coronal images. In fact, the contribution of wellknown physical causes leading to deviation of the measured polarization direction from the tangential direction is in the range of 1 -2 degrees at R ≤ 2R o (Molodensky, 1973;Molodenskii et al, 2009). distributions of the total polarization degree P KF (L) in these structures, passing through the centers of structures near the Sun; (c) "trajectories" from which distributions of the polarization degree were deduced; (d) comparison between our P KF (L) distributions in the plume and inter-plume regions, and those in the plume (star) and inter-plumes (cross) for the eclipse of 3 November 1994 (Koutchmy, 1994).…”

Section: Polarization Directionmentioning

confidence: 99%

White-Light Observations and Polarimetric Analysis of the Solar Corona During the Eclipse of 1 August 2008

et al. 2011

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In order to study the solar corona during eclipses, a new telescope was constructed. Three coronal images were obtained simultaneously through a single objective of the telescope as the coronal radiation passed through three polarizers (whose transmission directions were turned 0°, 60°, and 120°in the chosen direction); one image was obtained without a polarizer. The telescope was used to observe the solar corona during the eclipse of 1 August 2008. We obtained the distributions of polarization brightness, K-corona brightness, the degree of K-corona polarization and the total polarization degree; the polarization direction, depending on the latitude and radius in the plane of the sky, was also obtained. We calculated the radial distributions of electron density depending on the latitude. The properties of all these distributions were compared for different coronal structures. We determined the temperature of the coronal plasma in different coronal structures assuming hydrostatic equilibrium.

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“…[] and Molodenskii et al . [] cited χ < 1–2° in the low K‐corona and possible appearance of large deviations for specific areas in the range > 1.5–2 R ⊙ caused by sky polarization. We note that cited results correspond to selected position angle cuts.…”

Section: Total Solar Eclipse As An Approachmentioning

confidence: 99%

“…According to Figure 4 by Ozkan et al, [2002], there are χ up to 15°i n the range < 1.5 R ⊙ for the corona of 11 August 1999. Koutchmy et al [1999] and Molodenskii et al [2009] cited χ < 1-2°in the low K-corona and possible appearance of large deviations for specific areas in the range > 1.5-2 R ⊙ caused by sky polarization. We note that cited results correspond to selected position angle cuts.…”

Section: High-precision 2-d Linear Polarimetrymentioning

confidence: 99%

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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The polarization of the solar corona on March 29, 2006

Cited by 7 publications

References 1 publication

Detection of polarization neutral points in observations of the combined corona and sky during the 21 August 2017 total solar eclipse

Detection of polarization neutral points in observations of the combined corona and sky during the 21 August 2017 total solar eclipse

White-Light Observations and Polarimetric Analysis of the Solar Corona During the Eclipse of 1 August 2008

Imaging the structure of the low K‐corona

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