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

• Dumont R.

  Observatoire de Bordeaux

• Renard J. B.

  LPCE-CNRS

• Levasseur-Regourd A. C.

  Aeronomie CNRS

• Weinberg J. L.

  MK Ind. LLC

書誌事項

タイトル別名

• Disentangling the main populations of t

抄録

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 = Ð(α)/m along each line of sight (LOS), (α being the phase angle, m the subsolar distance of the LOS, Ð 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, Ð(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 cos¹² β_??_ function. The resulting brightness ratio at ε < 90°, which should be equal to ∫LOS cos¹² β(α) Ð(α)·d α/∫LOS Ð(α)dαLOS LOS turns out to be much lower than the ratio observed in the 60° > ε > 15° range (again ≈ 0.3). This contradiction is solved with a steeper exponent (20-22?) for cos β_??_, 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°.

収録刊行物

• Ｅａｒｔｈ，　Ｐｌａｎｅｔｓ　ａｎｄ　Ｓｐａｃｅ

  Ｅａｒｔｈ，　Ｐｌａｎｅｔｓ　ａｎｄ　Ｓｐａｃｅ 50 (6-7), 473-476, 1998

  地球電磁気・地球惑星圏学会 、公益社団法人 日本地震学会、特定非営利活動法人 日本火山学会、日本測地学会、日本惑星科学会

キーワード

• Space and Planetary Science
• Geology

詳細情報

• CRID: 1390282681485554944
• NII論文ID: 10002206850
• NII論文ID: 130003780723
• NII書誌ID: AA11211921
• DOI: 10.1186/bf03352136
• ISSN: 18805981
• ISSN: 13438832
• NDL書誌ID: 4552197
• Web Site: https://ndlsearch.ndl.go.jp/books/R000000004-I4552197
• Web Site: https://link.springer.com/content/pdf/10.1186/BF03352136.pdf
• Web Site: https://link.springer.com/article/10.1186/BF03352136/fulltext.html
• Web Site: http://link.springer.com/content/pdf/10.1186/BF03352136
• 本文言語コード: en
• データソース種別:
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  • NDL
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