The Zodiacal Light

Blackwell, D. E.; Dewhirst, David W.; Ingham, M. F.

doi:10.1016/b978-1-4831-9923-8.50006-1

Cited by 28 publications

(22 citation statements)

References 60 publications

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“…In general, it should be emphasized that small uncertainties in the determination of the strongly polarized K -coronal brightness have a drastic influence on the derived F-coronal polarization. Mann (1992) has attempted to derive the local properties of near-solar dust particles from the model of Blackwell et al (1967) and has concluded that the local polarization of the near-solar dust grains located at heliocentric distances smaller than r = 0.1 AU has a radial slope between r 2.8 and r 2.6 depending on model assumptions. On the other hand, the local polarization of the zodiacal light at visible wavelength has been derived by the nodes of lesser uncertainty method (see Levasseur-Regourd (1996) for a review).…”

Section: Polarization Of the F-coronamentioning

confidence: 99%

“…Blackwell and Petford (1966b) obtained the polarization of the F-corona to be almost zero at elongations ranging from 10 to 16 R , although two independent measurements at different eclipses of 1954 and 1963 were used for separation of the K -and F-corona. Blackwell et al (1967) have modeled the F-coronal polarization from 5 to 16 R at visible wavelength so that the model polarization can smoothly connect the polarization data of Blackwell and Petford (1966b). Assuming the K -coronal polarization to be constant beyond 5 R , Koutchmy and Lamy (1985) also have established a model of the F-coronal polarization, but there is a large difference by order of magnitude between the two models mentioned above.…”

Section: Polarization Of the F-coronamentioning

confidence: 99%

“…In the classical approach, the solar corona has been studied on the basis of its brightness, polarization, and color mainly in the visible wavelengths (see Blackwell et al, 1967). Since the sixties, further information has been obtained from nearinfrared observations (Peterson, 1967(Peterson, , 1969MacQueen, 1968), and with infrared imaging systems in the nineties (Hodapp et al, 1992;Kuhn et al, 1994;Tollestrup et al, 1994).…”

Section: Introductionmentioning

confidence: 99%

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Brightness of the solar F-corona

Kimura

Mann

2014

Earth Planet Sp

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We discuss our present knowledge about the brightness of the solar F-corona in the wavelength range from the visible to the middle infrared. From the general trend of the observational data, the F-corona is regarded as the continuous extension of the zodiacal light at smaller elongation of the line of sight. A contribution of thermal emission from dust is indicated by the increasing F-coronal brightness in comparison to the solar spectrum towards longer wavelength. As compared with the F-coronal brightness, the polarization and color in the visible regime are not well determined due to the high sensitivity of these quantities to the observational accuracy. Aside from observational problems, our present interpretation of the F-coronal brightness is also limited due to ambiguities in the inversion of the line of sight integral. Nevertheless, the measurements and model calculations of the brightness can be used to deduce some physical properties of dust grains. We show that the hump of the near-infrared brightness at 4 solar radii, which was sometimes observed in the corona, is related rather to the physical properties of dust grains along the line of sight than to the existence of a dust ring as previously discussed. We also show that the appearance or disappearance of the near-infrared peak in the coronal brightness cannot be described in any periodic cycle for each wavelength range.

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Section: Polarization Of the F-coronamentioning

confidence: 99%

Section: Polarization Of the F-coronamentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Brightness of the solar F-corona

Kimura

Mann

2014

Earth Planet Sp

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“…This light first manifests itself in early evening as a diffuse wedge of light in the southwestern horizon and gradually broadens with time. During the course of the night the zodiacal light becomes wider and more upright, although its position relative to the stars shifts only slightly [2].…”

Section: Zodiacal Lightmentioning

confidence: 99%

A physically-based night sky model

Jensen

Durand

Dorsey

et al. 2001

Proceedings of the 28th Annual Conference on Computer Graphics and Interactive Techniques

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This paper presents a physically-based model of the night sky for realistic image synthesis. We model both the direct appearance of the night sky and the illumination coming from the Moon, the stars, the zodiacal light, and the atmosphere. To accurately predict the appearance of night scenes we use physically-based astronomical data, both for position and radiometry. The Moon is simulated as a geometric model illuminated by the Sun, using recently measured elevation and albedo maps, as well as a specialized BRDF. For visible stars, we include the position, magnitude, and temperature of the star, while for the Milky Way and other nebulae we use a processed photograph. Zodiacal light due to scattering in the dust covering the solar system, galactic light, and airglow due to light emission of the atmosphere are simulated from measured data. We couple these components with an accurate simulation of the atmosphere. To demonstrate our model, we show a variety of night scenes rendered with a Monte Carlo ray tracer.

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“…The current state of knowledge of the F corona and its optical/IR properties, including polarization, is reviewed in Kimura & Mann (1998). There is more discussion of dust physics in Blackwell et al (1967a) and Mann et al (2004). Ragot & Kahler (2003) consider interactions of dust with CMEs.…”

Section: Introductionmentioning

confidence: 99%

On the Use of Total Brightness Measurements for Tomography of the Solar Corona

Frazin

Kamalabadi

2005

ApJ

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A time series of polarized white light coronagraph images may be used to make a tomographic estimate of the electron density (N e ) in three dimensions, as has been demonstrated by several authors. This technique has come to be known as solar rotational tomography (SRT). SRT relies on the fact that the polarized brightness ( pB) is dominated by the electron-scattered K corona. In contrast, the total brightness contains a large contribution from the dust-scattered F-corona with some signal from the K corona. The K-corona contribution to the total brightness (B) is of interest because the Thomson scattering has different angular dependences for the polarized and unpolarized components. This difference in angular dependence in principle allows one to exploit total brightness measurements as a source of independent information for SRT. In this paper the problem of making optimal tomographic estimates of N e using both total and polarized brightness data is considered under the assumption that the F-corona contribution can be determined with a known level of precision. Formulae for the reconstructions and the likely errors are given in terms of the singular value decomposition of the weighted measurement operators. It is shown that in order for the total brightness measurements to be useful for SRT, the process of removing the F-corona contribution must be almost perfect in the sense that it contributes uncertainty that is not much greater than the measurement noise in the polarized images. This result holds at heights below roughly 15 solar radii, where the F corona is almost completely unpolarized.

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The Zodiacal Light

Cited by 28 publications

References 60 publications

Brightness of the solar F-corona

Brightness of the solar F-corona

A physically-based night sky model

On the Use of Total Brightness Measurements for Tomography of the Solar Corona

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