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The Sun
The Sun

... According to Wien’s Law, 2,900,000/Temp in Kelvin, the peak emission of the sun is 2,900,000/6000K. This is equal to 483 nm, the color of blue-green light. This is why our eyes have evolved to detect the visible spectrum. ...
Astronomy
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... energy), it can go into orbit. For a satellite around Earth in low Earth orbit, this is about 8 km/s. ...
"The Probability and Effects of an Asteroid Impact with Earth"
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... at the expense of the mechanical energy of the shock, and is quickly dissipated. The constant replenishment of rising gas bubbles from the convection zone produces a constant source of shock heating in the gases lying above the solar photosphere, i.e. in the solar chromosphere. ...
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... equator. It is a projection of the Earth's equator out to the celestial sphere. The number of degrees that a celestial object is north or south of the celestial equator is called the declination (DEC) It is the analogue of latitude on the sky. The analogue of longitude is called right ascension (RA) ...
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... •  Assuming  a  value  of  T0  ,  the  temperature  at  the  center  of  the  disk   (not  at  the  center  of  the  Sun!),  one  can  then  determine  a  series  of   values  of  T  vs.  τ  and  thus  provide  informaCon  ab ...
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... Most  places  outside  the  tropics  have  four  distinct  seasons:  winter,  spring,  summer,   and  autumn.  But  there  are  great  differences  in  temperature  from  place  to  place.  For   instance,  it  is  warmer  near  the  eq ...
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... solar neighborhood, will occasionally result in close encounters between the Sun and other stars. Using the foregoing value for the density of stars in the solar neighborhood, one can predict that about 12 star systems (single or multiple stars) will pass within 1 pc of the Sun per million years. Th ...
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... 23h12m11s and declination written as, e.g. -40o12’13” • In this format, the m (’) and s (’’) are minutes and seconds of time (of arc) where a m is 1/60 of an hour (’ is 1/60 a degree) and a s (’’) is 1/60 of a minute (’) • To convert a dec of, e.g., -40o12m13s to degrees: – δ (degrees)= -1 x (40 + ( ...
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Tropical year

A tropical year (also known as a solar year), for general purposes, is the time that the Sun takes to return to the same position in the cycle of seasons, as seen from Earth; for example, the time from vernal equinox to vernal equinox, or from summer solstice to summer solstice. Because of the precession of the equinoxes, the seasonal cycle does not remain exactly synchronized with the position of the Earth in its orbit around the Sun. As a consequence, the tropical year is about 20 minutes shorter than the time it takes Earth to complete one full orbit around the Sun as measured with respect to the fixed stars (the sidereal year).Since antiquity, astronomers have progressively refined the definition of the tropical year. The Astronomical Almanac Online Glossary 2015 states:year, tropical:the period of time for the ecliptic longitude of the Sun to increase 360 degrees. Since the Sun's ecliptic longitude is measured with respect to the equinox, the tropical year comprises a complete cycle of seasons, and its length is approximated in the long term by the civil (Gregorian) calendar. The mean tropical year is approximately 365 days, 5 hours, 48 minutes, 45 seconds.An equivalent, more descriptive, definition is ""The natural basis for computing passing tropical years is the mean longitude of the Sun reckoned from the precessionally moving equinox (the dynamical equinox or equinox of date). Whenever the longitude reaches a multiple of 360 degrees the mean Sun crosses the vernal equinox and a new tropical year begins"". (Borkowski 1991, p. 122)The mean tropical year on January 1, 2000, was about 365.2421897 ephemeris days according to the calculation of Laskar (1986); each ephemeris day lasting 86,400 SI seconds. By 2010 this had decreased to 365.2421891 (365 ephemeris days, 5 hours, 48 minutes and 45.14 seconds). This is about 365.242181 mean solar days, though the length of a mean solar day is constantly changing.
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