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Laboratory Procedure (Word Format)
Laboratory Procedure (Word Format)

... The angular distance an object is above or below the celestial equator is called declination. Declination ranges from 0o (object on the celestial equator) to +90o (object at the NCP) or to -90o (object at the SCP). Many objects could be located at the same declination, so we must now make a measure ...
The Sun - Sheldon ISD
The Sun - Sheldon ISD

... The Sun is made up of several layers. It has a core. Next is the radiation zone. Above that is the convection zone. The "surface" of the sun is called the photosphere. Above the surface are two layers of gas. They are called the chromosphere and the corona. There is no real surface on the sun. It is ...
Paper (pdf)
Paper (pdf)

... 7◦ of 45◦ , so that the difference in s- and p-polarization reflectivity is maximized. As with the first concept, a multilayer coating on the mirror increases the 0.25 keV reflectivity to about 10% (depending on the surface roughness) and defines the bandwidth of the telescope. As shown in Figure 1 ...
Polarization of x-gamma radiation produced by a Thomson and
Polarization of x-gamma radiation produced by a Thomson and

... A systematic study of the polarization of x-gamma rays produced in Thomson and Compton scattering is presented, in both classical and quantum schemes. Numerical results and analytical considerations let us to establish the polarization level as a function of acceptance, bandwidth and energy. Few sou ...
digital book, stars and planets
digital book, stars and planets

... more than four billion years for the Sun to burn out. Earth receives just the right amount of warmth and light from the Sun. If we were closer to the Sun, ...
PPTX
PPTX

... • Light travel time distances calculated from the synchrotron cooling timescales. ...
X-ray polarimetry in Xenon gas filled detectors
X-ray polarimetry in Xenon gas filled detectors

... preferentially aligned with the polarization vector;  unpolarized X-rays: d   1  1  P cos    (  1  sin 2  ) cos   ...
Size in Astronomy Often….angular size
Size in Astronomy Often….angular size

...  Remember: Earth is 1 AU from sun……and 1 AU = 1.5 x 1011 meters.  What’s the angular size of Jupiter as viewed from the earth at “opposition” (when we’re both on the same side of the sun)? ...
Lecture 2
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... The 'Equation of Time' Days in our Winter are thus slightly shorter than 24 hours, while days in Summer are slightly longer than 24 hours. This means that if you measured the exact time at which the Sun was due south every day, you would find that your 'clock' based on this was not quite accurate, ...
SOFIA Polarimetry: Recent Musings
SOFIA Polarimetry: Recent Musings

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The SUN - MindMeister
The SUN - MindMeister

... social studies and global studies. It is most appropriate for high school students but is suitable for middle school students as well. The series can be used as a companion to the Big History Project online course and curriculum. (Visit www.bighistoryproject.com to learn more.) ...
Circular Polarization in Star- Formation Regions
Circular Polarization in Star- Formation Regions

... Because of the high obscuration, these regions are directly observable only at IR and radio wavelengths, whereas the circular dichroism bands in amino acids and similar molecules are in the UV at wavelengths of about 200 to 250 nm. We therefore investigated whether the mechanism responsible for the ...
angular size
angular size

... – a body of related hypotheses can be pieced together into a self consistent description of nature  Laws of Physics – theories that accurately describe the workings of physical reality, have stood the test of time and been shown to have great and general validity ...
Our Very Own Star: The Sun - cmase
Our Very Own Star: The Sun - cmase

... When you look at the night sky filled with stars, have you ever wondered what a star is? Walk outside on a clear day and say, "Hello!" to our very own star - the Sun! (But don’t ever look directly at the Sun. You may damage your eyes.) ...
Model - High Energy Astrophysics Group
Model - High Energy Astrophysics Group

... in wide energy bands (optical to GeV). We examine the polarization characteristics predicted by the synchrotron model ...
Catherine and Puti 7F
Catherine and Puti 7F

... The sun spots We don't often think of the Sun as having cooler areas on its surface. The Sun is too hot for an astronaut to go on the sun, but there are areas which are a bit cooler than others. These areas are called sun spots. Sun spots are still very hot. However, because they are a bit cooler t ...
10Sept_2014
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... • Since earliest times, humans have sought to understand the night sky • A useful model of the sky is called the Celestial Sphere • It is not real – it is simply a tool for understanding and prediction ...
March/April 2015
March/April 2015

... Sun, certain wavelengths are absorbed by the elements in the Sun’s atmosphere. The atmosphere is full of atoms and molecules, and particular wavelengths of the passing light will happily interact with some of these atoms and excite their electrons. While some wavelengths are absorbed, all the other ...
The Sun - MrsAllisonMagee
The Sun - MrsAllisonMagee

... • Nuclear Fusion: the process by which nuclei of small atoms combine to form a new, more massive nucleus, which results in large amounts of energy being released. • Nuclear fusion produces the sun’s energy. • In our sun hydrogen fuses into helium. ...
Observing the Sky
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... – lowest place you see the sky – Shape: a circle (you are at the center) – Location: halfway between Zenith and Nadir ...
Celestial Mechanics Fun with Kepler and Newton
Celestial Mechanics Fun with Kepler and Newton

... •The Sun’s motion across the sky changes over the course of the year. This is due mainly to the tilt of the Earth’s rotation axis. •The maximum angular height above the horizon at a location in the Northern Hemisphere is maximum on the Summer Solstice and minimum on the Winter Solstice. This results ...
Polarization
Polarization

...  The major and minor axes respectively of the ellipse. ...
Our Star the Sun
Our Star the Sun

... atmosphere and can extend far into space. It can only be seen during an eclipse. ...
McConnell XGPolarimetry SSE
McConnell XGPolarimetry SSE

... Gamma-ray bursts (GRBs) are brief, energetic bursts of gamma-rays that mark the most violent, cataclysmic explosions in the universe. Extensive multi-wavelength observations of GRBs and their long-wavelength Figure 4: Two types of GRB models [5]: (a) the physical afterglows have revealed the followi ...
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Rayleigh sky model



The Rayleigh sky model describes the observed polarization pattern of the daytime sky. Within the atmosphere Rayleigh scattering of light from air molecules, water, dust, and aerosols causes the sky's light to have a defined polarization pattern. The same elastic scattering processes cause the sky to be blue. The polarization is characterized at each wavelength by its degree of polarization, and orientation (the e-vector angle, or scattering angle).The polarization pattern of the sky is dependent on the celestial position of the sun. While all scattered light is polarized to some extent, light is highly polarized at a scattering angle of 90° from the light source. In most cases the light source is the sun, but the moon creates the same pattern as well. The degree of polarization first increases with increasing distance from the sun, and then decreases toward the anti-sun. Thus, the maximum degree of polarization occurs in a circular band 90° from the sun. In this band, degrees of polarization near 80% are typically reached.When the sun is located at the zenith, the band of maximal polarization wraps around the horizon. Light from the sky is polarized horizontally along the horizon. During twilight at either the Vernal or Autumnal equinox, the band of maximal polarization is defined by the North-Zenith-South plane, or meridian. In particular, the polarization is vertical at the horizon in the North and South, where the meridian meets the horizon. The polarization at twilight at an equinox is represented by the figure to the right. The red band represents the circle in the North-Zenith-South plane where the sky is highly polarized. The cardinal directions N, E, S, W are shown at 12-o'clock, 9 o'clock, 6 o'clock and 3 o'clock (counter-clockwise around the celestial sphere since the observer is looking up at the sky).Note that because the polarization pattern is dependent on the sun, it changes not only throughout the day but throughout the year. When the sun sets toward the South, in the winter, the North-Zenith-South plane is offset, with ""effective"" North actually located somewhat toward the West. Thus if the sun sets at an azimuth of 255° (15° South of West) the polarization pattern will be at its maximum along the horizon at an azimuth of 345° (15° West of North) and 165° (15° East of South).During a single day, the pattern rotates with the changing position of the sun. At twilight it typically appears about 45 minutes before local sunrise and disappears 45 minutes after local sunset. Once established it is very stable, showing change only in its rotation. It can easily be seen on any given day using polarized sunglasses.Many animals use the polarization patterns of the sky at twilight and throughout the day as a navigation tool. Because it is determined purely by the position of the sun, it is easily used as a compass for animal orientation. By orienting themselves with respect to the polarization patterns, animals can locate the sun and thus determine the cardinal directions.
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