Numerical Calculation and Analysis of Mie Scattering Phase Function of Nucleated Cells

2017 ◽  
Vol 44 (8) ◽  
pp. 0807003
Author(s):  
卜 敏 Bu Min ◽  
胡双双 Hu Shuangshuang ◽  
陆 伟 Lu Wei ◽  
金卫凤 Jin Weifeng ◽  
王亚伟 Wang Yawei
Keyword(s):  
Numerical Calculation ◽  
Phase Function ◽  
Mie Scattering ◽  
Scattering Phase ◽  
Scattering Phase Function

scholarly journals Power Series Expansion of the Mie Scattering Phase Function

1983 ◽  
Vol 36 (5) ◽  
pp. 701 ◽  
Author(s):  
Michael A Box
Keyword(s):  
Power Series ◽  
Phase Function ◽  
Power Series Expansion ◽  
Mie Scattering ◽  
Matrix Elements ◽  
Dust Clouds ◽  
Power Series Expansions ◽  
Scattering Phase ◽  
Natural Variable ◽  
Scattering Phase Function

We develop power series expansions for both the Mie theory scattering amplitudes and the scattering phase matrix elements in terms of the variable s = sin2W, where () is the scattering angle. It is easily seen that s is the natural variable for such expansions. These expansions should prove particularly useful whenever the forward diffraction peak, rather than the entire phase function, is of primary interest. Possible applications include the analysis of solar aureole data and the modelling of laser beam propagation in fogs and dust clouds.

A Comparison of Aphelion Cloud Belt Phase Functions Before and After the Mars Year 34 Global Dust Storm

2021 ◽  
Author(s):  
Alex Innanen ◽  
Brittney Cooper ◽  
Charissa Campbell ◽  
Scott Guzewich ◽  
Jacob Kloos ◽  
...  
Keyword(s):  
Dust Storm ◽  
Phase Function ◽  
Dust Storms ◽  
Ice Crystal ◽  
Ice Clouds ◽  
Water Ice ◽  
Ice Cloud ◽  
Sky Survey ◽  
Scattering Phase ◽  
Scattering Phase Function

<p>1. INTRODUCTION</p><p>The Mars Science Laboratory (MSL) is located in Gale Crater (4.5°S, 137.4°E), and has been performing cloud observations for the entirety of its mission, since its landing in 2012 [eg. 1,2,3]. One such observation is the Phase Function Sky Survey (PFSS), developed by Cooper et al [3] and instituted in Mars Year (MY) 34 to determine the scattering phase function of Martian water-ice clouds. The clouds of interest form during the Aphelion Cloud Belt (ACB) season (L<sub>s</sub>=50°-150°), a period of time during which there is an increase in the formation of water-ice clouds around the Martian equator [4]. The PFSS observation was also performed during the MY 35 ACB season and the current MY 36 ACB season.</p><p>Following the MY 34 ACB season, Mars experienced a global dust storm which lasted from L<sub>s</sub>~188° to L<sub>s</sub>~250° of that Mars year [5]. Global dust storms are planet-encircling storms which occur every few Mars years and can significantly impact the atmosphere leading to increased dust aerosol sizes [6], an increase in middle atmosphere water vapour [7], and the formation of unseasonal water-ice clouds [8]. While the decrease in visibility during the global dust storm itself made cloud observation difficult, comparing the scattering phase function prior to and following the global dust storm can help to understand the long-term impacts of global dust storms on water-ice clouds.</p><p>2. METHODS</p><p>The PFSS consists of 9 cloud movies of three frames each, taken using MSL’s navigation cameras, at a variety of pointings in order to observe a large range of scattering angles. The goal of the PFSS is to characterise the scattering properties of water-ice clouds and to determine ice crystal geometry.  In each movie, clouds are identified using mean frame subtraction, and the phase function is computed using the formula derived by Cooper et al [3]. An average phase function can then be computed for the entirety of the ACB season.</p><p><img src="https://contentmanager.copernicus.org/fileStorageProxy.php?f=gnp.eda718c85da062913791261/sdaolpUECMynit/1202CSPE&app=m&a=0&c=67584351a5c2fde95856e0760f04bbf3&ct=x&pn=gnp.elif&d=1" alt="Figure 1 – Temporal Distribution of Phase Function Sky Survey Observations for Mars Years 34 and 35" width="800" height="681"></p><p>Figure 1 shows the temporal distributions of PFSS observations taken during MYs 34 and 35. We aim to capture both morning and afternoon observations in order to study any diurnal variability in water-ice clouds.</p><p>3. RESULTS AND DISCUSSION</p><p>There were a total of 26 PFSS observations taken in MY 35 between L<sub>s</sub>~50°-160°, evenly distributed between AM and PM observations. Typically, times further from local noon (i.e. earlier in the morning or later in the afternoon) show stronger cloud features, and run less risk of being obscured by the presence of the sun. In all movies in which clouds are detected, a phase function can be calculated, and an average phase function determined for the whole ACB season.  </p><p>Future work will look at the water-ice cloud scattering properties for the MY 36 ACB season, allowing us to get more information about the interannual variability of the ACB and to further constrain the ice crystal habit. The PFSS observations will not only assist in our understanding of the long-term atmospheric impacts of global dust storms but also add to a more complete image of time-varying water-ice cloud properties.</p>

Aerosol Scattering Phase Function and Visibility Based on Charge Coupled Device

2012 ◽  
Vol 32 (9) ◽  
pp. 0901001
Author(s):  
孟祥谦 Meng Xiangqian ◽  
胡顺星 Hu Shunxing ◽  
王英俭 Wang Yingjian ◽  
胡欢陵 Hu Huanling
Keyword(s):  
Phase Function ◽  
Charge Coupled Device ◽  
Aerosol Scattering ◽  
Scattering Phase ◽  
Scattering Phase Function
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