Astronomy
Measurements of the zenith distance or altitude of the sun at noon (ie, at the time of upper culmination) at the same latitude was found that the declination of the sun throughout the year varies between 23 e 27 'up-23e27' twice a year passing through zero. From observations of the night sky kind of change that, and right ascension of the sun throughout the year and gradually changes from 0 ? to 360e, or from 0h to 24h. Indeed, at midnight, at the top are the culmination of the stars, right ascensions of which differ from the right ascension of the sun on the 180e or 12h. The observations also show that every day at midnight stars culminate with more and more direct ascent, consequently, the right ascension of the sun each day increases. Considering the continuous change of both the origin of the sun, it is easy to install, it moves among the stars from west to east along the great circle of the celestial sphere, called the ecliptic. The plane of the ecliptic E'' ^ E d (11) is inclined to the plane of the celestial equator at an angle e = 23rd 27 '. The diameter of PP ', perpendicular to the plane of the ecliptic, the ecliptic is called the axis and intersects with the surface of the celestial sphere in the ecliptic north pole P (which lies in the northern hemisphere) and south pole of the ecliptic P' (in the Southern Hemisphere). The ecliptic intersects the celestial equator at two points: at the vernal equinox ^ and at the autumnal equinox d. At the point of the vernal equinox ^ Sun crosses the celestial equator, moving from the southern hemisphere to the northern celestial sphere. At point d the autumnal equinox the Sun moves from the northern to the southern hemisphere. Point of the ecliptic, are separated from the equinoctial to the 90s, called the point of the summer solstice (northern hemisphere) and the point of the winter solstice (Southern Hemisphere). Large semi-circle of the celestial sphere PMP ', passing through the ecliptic poles and through the M star, is called the circle of latitude star. The ecliptic and the vernal equinox are the basis of the ecliptic celestial coordinate system. One coordinate in this system is the ecliptic latitude b luminaries M, which is called the arc of a circle of latitude mM (see 11) of the ecliptic to the celestial body, or the central angle between the plane of the ecliptic TOM and the direction of light M. Ecliptic latitude are measured in the range from 0 ? to + 90
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Astronomy
The ecliptic. Ecliptic coordinate system
- Cassini Finds Titan's Clouds Hang On To Summer
Cloud chasers studying Saturn's moon Titan say its clouds form and move much like those on Earth, but in a much slower, more lingering fashion. Their forecast for Titan's early autumn -- warm and wetter. Scientists with NASA's Cassini mission...
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When the light comes and goes, its z = 90 °, h = 0e, and the azimuths of the points of sunrise and sunset depend on the declination and the latitude of the place lights up. At the time of upper culmination zenith distance of the light of the minimum,...
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At what point would the Earth's surface, we are, we always think that all the heavenly bodies are to us at the same distance on the inner surface of a sphere, which is commonly called the firmament, or just air. Day of the sky, if it is not covered...
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About every 15 Earth years, Saturn?s experiences an equinox, much like Earth?s equinox. On Earth it occurs twice in Earth?s orbit?two times every Earth year?when the Sun lies in the Earth?s equatorial plane. As a result, the duration of day and night...
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If you are curious to know about Ultraviolet astronomy, then go through the following article on ultraviolet astronomy. Astronomy is one of the oldest science. Astronomy is the name of a unique scientific study of celestial objects like stars, planets...
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