scholarly journals Zodiacal Light Beyond Earth Orbit Observed with Pioneer 10

2018 ◽  
Vol 156 (3) ◽  
pp. 86 ◽  
Author(s):  
T. Matsumoto ◽  
K. Tsumura ◽  
Y. Matsuoka ◽  
J. Pyo
Keyword(s):  
Earth Orbit ◽  
Zodiacal Light ◽  
Pioneer 10

scholarly journals The Change in Near-Ecliptic Zodiacal Light Brightness with Heliocentric Distance

1985 ◽  
Vol 85 ◽  
pp. 21-25
Author(s):  
G.N. Toller ◽  
J.L. Weinberg
Keyword(s):  
Heliocentric Distance ◽  
Asteroid Belt ◽  
Zodiacal Light ◽  
The Earth ◽  
Pioneer 10

AbstractBackground starlight observed by the Pioneer 10 Imaging Photopolarimeter from beyond the asteroid belt is used to isolate zodiacal light in Pioneer observations at heliocentric distances R between 1 and 3 AU. Near-ecliptic zodiacal light brightness data in the range 65° to 180° elongation ε are used to depict changes in the shape of the zodiacal light with ε and R and are compared to the corresponding views seen from the Earth and from the Helios 1 and 2 spacecraft.

scholarly journals Brightness and Polarization of the Zodiacal Light: Results of Fixed-Position Observations from Skylab

1980 ◽  
Vol 90 ◽  
pp. 19-22
Author(s):  
J. L. Weinberg ◽  
R. C. Hahn
Keyword(s):  
Asteroid Belt ◽  
Degree Of Polarization ◽  
Zodiacal Light ◽  
Fixed Position ◽  
Vernal Equinox ◽  
The North ◽  
Celestial Pole ◽  
Total Light ◽  
North Galactic ◽  
Pioneer 10

In an earlier paper Sparrow et al. (1976) found the polarized brightness of zodiacal light to have solar color at five sky positions for which there were fixed-position observations from Skylab: north celestial pole, south ecliptic pole, vernal equinox, and two places near the north galactic pole. The brightness and degree of polarization of zodiacal light at these sky positions are derived using Pioneer 10 observations of background starlight from beyond the asteroid belt (Weinberg et al., 1974; Schuerman et al., 1976) and the assumption that the zodiacal light is also solar color in total light.

scholarly journals Fitting Zodiacal Models

2001 ◽  
Vol 204 ◽  
pp. 157-160 ◽  
Author(s):  
Edward L. Wright
Keyword(s):  
Solar System ◽  
Radiation Field ◽  
Measured Data ◽  
Low Earth Orbit ◽  
Earth Orbit ◽  
Zodiacal Light ◽  
Extragalactic Background Light ◽  
Background Light

Models of the zodiacal light are necessary to convert measured data taken from low Earth orbit into the radiation field outside the Solar System. The uncertainty in these models dominates the overall uncertainty in determining the extragalactic background light for wavelengths λ < 100 μm.

scholarly journals Evidence that the Properties of Interplanetary Dust Beyond 1 AU are Not Homogeneous

1980 ◽  
Vol 90 ◽  
pp. 71-74 ◽  
Author(s):  
Donald W. Schuerman
Keyword(s):  
Cross Section ◽  
Heliocentric Distance ◽  
Interplanetary Dust ◽  
Scattering Cross Section ◽  
Zodiacal Light ◽  
Dust Density ◽  
Scattering Cross ◽  
Pioneer 10

Traditionally, earth-based observations of the zodiacal light (ZL) require two assumptions for further analysis: (A1) the dust density (n) is a power of heliocentric distance (R), n ∝ R−ν; (A2) the nature (scattering cross section, σ) of the dust is independent of location, σ(r,h,θ)=σ(θ). Observations from Pioneer 10 do not verify these assumptions.

scholarly journals Dynamics of Micrometeoroids

1980 ◽  
Vol 90 ◽  
pp. 293-298 ◽  
Author(s):  
E. Grün ◽  
H. A. Zook
Keyword(s):  
Heliocentric Distance ◽  
Ecliptic Plane ◽  
Interplanetary Dust ◽  
Spatial Density ◽  
Orbital Elements ◽  
Zodiacal Light ◽  
Consistent Picture ◽  
Time Variations ◽  
Pioneer 10

Recent observations of zodiacal light have established a reliable and consistent picture of the spatial distribution of interplanetary dust in the ecliptic plane. The spatial density nr varies with heliocentric distance r according to a power law nr ∝ r−ν. From Helios observations an exponent v = 1.3 is derived for the distance interval from 0.08 A.U. to 1 A.U. (Link et al. 1976). Outside the earth's orbit the Pioneer 10 and 11 results suggest a higher exponent v = 1.5 for the distance interval from 1 A.U. to 3.3. A.U. (Hanner et al., 1976). Giese and Grün (1976) showed that the results from zodiacal light observations are compatible with the micrometeoroid fluxes derived from in situ measurements and lunar crater statistics. They found that micrometeoroids in the size range from 10 μm to 100 μm radii (corresponding roughly to 10−8g to 10−5g) contribute most to the zodiacal light brightness.The orbital distribution of large interplanetary particles (10−6 g < m < 10−3g) is known from meteor observations. Sekanina and Southworth (1975) reported average orbital elements of these particles: ā ∼ 1.25 A.U., ē ∼ 0.4 and ī ∼ 20°. Orbital information on micrometeoroids (m < 10−8g) is obtained from in situ detectors on board the Pioneer 8 and 9 and Helios 1 spaceprobes and the HEOS-2 satellite. Characteristics of the different micrometeoroid experiments are given in Table 1. There is almost no time overlap in the data taking intervals of the experiments. Therefore one has to assume that there are no time variations of the meteoroid flux on the time scale of 1 to 10 years if one compares the results from the different experiments. This assumption may be violated for the smallest of the observed particles (m < 10−13g) due to strong electromagnetic interaction of these particles with the interplanetary magnetic field (Morfill and Grün 1979).

Zodiacal light and the asteroid belt: The view from Pioneer 10

1974 ◽  
Vol 79 (25) ◽  
pp. 3671-3675 ◽  
Author(s):  
M. S. Hanner ◽  
J. L. Weinberg ◽  
L. M. DeShields ◽  
B. A. Green ◽  
G. N. Toller
Keyword(s):  
Asteroid Belt ◽  
Zodiacal Light ◽  
Pioneer 10

scholarly journals A Search for Small Scale Structures in the Zodiacal Light

1985 ◽  
Vol 85 ◽  
pp. 33-37
Author(s):  
S.S. Hong ◽  
N.Y. Misconi ◽  
M.H.H. van Dijk ◽  
J.L. Weinberg ◽  
G.N. Toller
Keyword(s):  
Brightness Distribution ◽  
Empirical Method ◽  
Asteroid Belt ◽  
Small Scale ◽  
High Angular Resolution ◽  
Zodiacal Light ◽  
Radiation Background ◽  
Scale Structures ◽  
Pioneer 10 ◽  
Small Scale Structures

AbstractGegenschein observations from Pioneer 10 were found to have brightness structures with an amplitude of about 10% and a period of several to ten degrees in elongation. A search is made for such structures in high angular resolution ground-based observations from Mt. Haleakala, Hawaii. A new empirical method is used to correct for atmosphere-originated radiation. Background starlight is subtracted using Pioneer 10 observations from beyond the asteroid belt. Preliminary analysis of the ground data also indicates the presence of small amplitude structures in the brightness distribution.

scholarly journals Light Scattering by Dust Particles in the Outer Solar System

1991 ◽  
Vol 126 ◽  
pp. 155-158
Author(s):  
J.W. Hovenier ◽  
P.B. Bosma
Keyword(s):  
Solar System ◽  
Cross Section ◽  
Particle Density ◽  
Interplanetary Dust ◽  
Dust Particles ◽  
Outer Solar System ◽  
Zodiacal Light ◽  
Particle Density Distribution ◽  
Photometric Observations ◽  
Pioneer 10

AbstractPhotometric observations of the zodiacal light performed by Pioneer 10 indicated that there may be very little scattering by dust in the outer solar system. To shed more light on this problem we formulate explicit expressions for interpreting the brightness observed by a spacecraft travelling inside or outside a finite homogeneous cloud of scattering particles. An application is made to the ecliptic zodiacal light brightness as observed by Pioneer 10 and tabulated by Toller and Weinberg (1985). A satisfactory interpretation of these data as well as earthbound observations can be given by means of a model having a particle density distribution or mean scattering cross section which vanishes beyond 2.8 - 3.7 AU. Some implications for the nature and spatial distribution of the interplanetary dust are discussed.

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