Phase function and polarization curve of interplanetary scatterers from zodiacal light photopolarimetry

Dumont, René

doi:10.1016/0032-0633(73)90189-x

Cited by 63 publications

(25 citation statements)

References 11 publications

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“…A common method of data analysis applies forward calculations of the line of sight integral under reasonable assumptions about particle properties and spatial distribution. Detailed descriptions of the line of sight integrals have been given before (see Dumont, 1973;Röser and Staude, 1978;Giese et al, 1986). Also the average scattering properties of particles have been directly inverted from the brightness integral in some cases (see for instance Levasseur-Regourd and Dumont, 1980;Lamy and Perrin, 1986).…”

Section: Brightness Inversion and Optical Propertiesmentioning

confidence: 99%

“…Dumont, 1973;Hong, 1985;Perrin and Lamy, 1989); in the case of thermal emission the VSF is replaced with a volume emission function, VEF (see below). Both the VSF and the VEF denote the average differential cross section dσ/d of particles per volume element for the process in question and include the spatial variation of particle number density.…”

Section: Brightness Inversion and Optical Propertiesmentioning

confidence: 99%

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Zodiacal Cloud Complexes

Mann

2014

Earth Planet Sp

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We discuss some aspects of the study of the Zodiacal cloud based on brightness observations. The discussion of optical properties as well as the spatial distribution of the dust cloud show that the description of the dust cloud as a homogeneous cloud is reasonable for the regions near the Earth orbit, but fails in the description of the dust in the inner solar system. The reasons for this are that different components of the dust cloud may have different types of orbital evolution depending on the parameters of their initial orbits. Also the collisional evolution of dust in the inner solar system may have some influence. As far as perspectives for future observations are concerned, the study of Doppler shifts of the Fraunhofer lines in the Zodiacal light will provide further knowledge about the orbital distribution of dust particles, as well as advanced infrared observations will help towards a better understanding of the outer solar system dust cloud beyond the asteroid belt.

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Section: Brightness Inversion and Optical Propertiesmentioning

confidence: 99%

Section: Brightness Inversion and Optical Propertiesmentioning

confidence: 99%

Zodiacal Cloud Complexes

Mann

2014

Earth Planet Sp

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“…Rigorous inversion is possible (Dumont, 1973) if the zodiacal cloud is assumed to be homogeneous (same properties everywhere, except density heliocentric-dependent by a power law r -n ), but this assumption turned out to be wrong when the Helios probes showed the polarisation degree (averaged along the line of sight-LOS) to change with spacecraft location.…”

Section: Introductionmentioning

confidence: 99%

Disentangling the main populations of the Zodiacal Cloud from Zodiacal Light observations

et al. 2014

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Photometric surveys of the Zodiacal Light (ZL) already allowed to retrieve features of interplanetary dust space distribution and optical behaviour. Of the brightness "gathering" function dZ = ᑞ(α)/m along each line of sight (LOS), (α being the phase angle, m the subsolar distance of the LOS, ᑞ the local scattering coefficient), two approximate values could be derived, based on the constraints provided by the two observed values of its integral Z, when the LOS is in-ecliptic. This "nodes of lesser uncertainty" method (Dumont, Levasseur-Regourd, Renard, 1985 to 1996, however, lowered but did not rule out question marks upon the phase function.To improve this inversion, additional constraints can be found in ZL surveys from deep space probes. We show that both the Pioneer 10 (Toller and Weinberg, 1985) and (despite their lack of in-ecliptic scans) the Helios (Leinert et al., 1982) data imply the phase function to weakly depart from isotropy, at least in the 30°-150° range.The latitudinal dependence f(β ᭪ , r = cst) of the space density (less well known than the heliocentric, ᑞ(r, β ᭪ = 0)) can be tracked through the brightness ratio, at the same elongation ε, aiming in the helioecliptic meridian, against in the ecliptic. At ε = 90°, this ratio 0.3 would lead-in the improper assumption of a single, homogeneous cloud-to fit the latitudinal density drop by a Ӎ cos 12 β ᭪ function. The resulting brightness ratio at ε < 90°, which should be equal to cos 12 β α α α α αturns out to be much lower than the ratio observed in the 60° > ε > 15° range (again Ӎ0.3). This contradiction is solved with a steeper exponent (20-22?) for cosβ ᭪ , and by assuming the flattened cloud to coexist with another one, spherically symmetrical, which contributes 15-25 S10 at ε = 90°, 50-80 S10 at ε = 60°, 100-160 S10 at ε = 45° and 250-450 S10 at ε = 30°.

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“…From ground base Zodiacal Light measurements and the experimental results of Pioneer X the density, p(r), and phase,a(6), functions are obtained without any previous assumptions about them.METHOD: In the present work we develop a method following Dumont(1973) in which (r,e) is detemined from a previously assumed Z(r,e) in the symmetry plane of the cloud where Z is taken to be a continuous and differentiable function of r and e.In the polar coordinate diagram (r,e) of fig.1 …”

mentioning

confidence: 99%

“…METHOD: In the present work we develop a method following Dumont(1973) in which (r,e) is detemined from a previously assumed Z(r,e) in the symmetry plane of the cloud where Z is taken to be a continuous and differentiable function of r and e.…”

mentioning

confidence: 99%

Method for the Determination of Density and Phase Functions of Interplanetary Dust

Mújica

López

Sánchez

1980

Symp. - Int. Astron. Union

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SUMMARY: A method of determination of the scattered light intensity, 3(r,e), by a unit-volume of interplanetary space is presented. From ground base Zodiacal Light measurements and the experimental results of Pioneer X the density, p(r), and phase,a(6), functions are obtained without any previous assumptions about them.METHOD: In the present work we develop a method following Dumont(1973) in which (r,e) is detemined from a previously assumed Z(r,e) in the symmetry plane of the cloud where Z is taken to be a continuous and differentiable function of r and e.In the polar coordinate diagram (r,e) of fig.1

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Phase function and polarization curve of interplanetary scatterers from zodiacal light photopolarimetry

Cited by 63 publications

References 11 publications

Zodiacal Cloud Complexes

Zodiacal Cloud Complexes

Disentangling the main populations of the Zodiacal Cloud from Zodiacal Light observations

Method for the Determination of Density and Phase Functions of Interplanetary Dust

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