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PRODID:IEEE vTools.Events//EN
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DTSTART:20190310T030000
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DTSTART:20181104T010000
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BEGIN:VEVENT
DTSTAMP:20181114T222042Z
UID:383E80B7-E105-4A48-8598-A6E68D86EF10
DTSTART;TZID=America/New_York:20181114T153000
DTEND;TZID=America/New_York:20181114T163000
DESCRIPTION:This talk will use measurements from an all-sky polarization im
 ager built at Montana State University\, along with an experimentally vali
 dated model\, to illustrate and explain how skylight polarization varies w
 ith time\, location\, and wavelength as a function of environmental parame
 ters. Scattering by atmospheric gas molecules produces strongly polarized 
 skylight\, but multiple scattering by clouds\, aerosols\, and the underlyi
 ng surface generally reduces that polarization at visible wavelengths. In 
 the shortwave infrared\, this process can be reversed\, with higher aeroso
 l content actually giving rise to a higher degree of polarization. These p
 rocesses lead to a band of maximum polarization stretching across the sky 
 at an angular location approximately 90 degrees from the Sun. This polariz
 ation pattern moves across the sky throughout the day\, with a degree of p
 olarization that varies with atmospheric and underlying surface conditions
 . Measurements also will be shown from the 21 August 2017 solar eclipse\, 
 during which we measured an instantaneous transition from the normal dayti
 me polarization pattern to one centered on the zenith during totality.\n\n
 Speaker(s): Joseph Shaw \, \n\nRoom: Carlson Auditorium\, Bldg: 76\, Roche
 ster Institute of Technology\, 54 Lomb Memorial Drive\, Rochester\, New Yo
 rk\, United States\, 14623
LOCATION:Room: Carlson Auditorium\, Bldg: 76\, Rochester Institute of Techn
 ology\, 54 Lomb Memorial Drive\, Rochester\, New York\, United States\, 14
 623
ORGANIZER:emmett@cis.rit.edu
SEQUENCE:3
SUMMARY:All-sky Imaging of Skylight Polarization
URL;VALUE=URI:https://events.vtools.ieee.org/m/180497
X-ALT-DESC:Description: <br /><p>This talk will use measurements from an al
 l-sky polarization imager built at Montana State University\, along with a
 n experimentally validated model\, to illustrate and explain how skylight 
 polarization&nbsp\;varies with time\, location\,&nbsp\;and wavelength as a
  function of environmental parameters.&nbsp\;Scattering by atmospheric gas
  molecules produces strongly polarized skylight\, but multiple scattering 
 by clouds\, aerosols\, and the underlying surface generally reduces that p
 olarization at visible wavelengths. In the shortwave infrared\, this proce
 ss can be reversed\, with higher aerosol content actually giving rise to a
  higher degree of polarization.&nbsp\;These processes&nbsp\;lead to a band
  of maximum polarization&nbsp\;stretching across the sky at an angular loc
 ation approximately 90&nbsp\;degrees from the Sun. This polarization patte
 rn&nbsp\;moves&nbsp\;across the sky throughout the day\, with a degree of 
 polarization that varies with atmospheric and underlying surface condition
 s. Measurements also will be shown from the 21 August 2017 solar eclipse\,
  during which we measured an instantaneous transition from the normal dayt
 ime polarization pattern to one centered on the zenith during totality.&nb
 sp\;</p>
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