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Regents Earth Science – Unit 5: Astronomy
Regents Earth Science – Unit 5: Astronomy

... Sun is at the center of the solar system and the Earth and other planets revolve around the Sun ...
Document
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... sun? More than 1 AU from the sun? How long does sunlight take to reach the Earth? 9. What is a comet? (p. 500) Where is the asteroid belt? (pg. 502) 10. What is the difference between a meteor, meteoroid and meteorite? P.503 ...
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... • Ships apparently rising up out of the sea or sinking into it • Lunar eclipses - the leading and trailing edge of the earth’s shadow were curved causing us to assume the object casting the shadow was round • As an observer increased altitude he could see farther over the earth’s curvature ...
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... Our sun is a star. Like all stars, it is a mass of very hot gases. It is matter in a state that is called plasma. (On Earth, most matter exists in one of three states: solid, liquid, or gas. On the sun, a fourth state of matter is found -- plasma.) On Earth, burning fossil fuels like gasoline or coa ...
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... 5. Describe how Earth’s orbit around the sun determines the seasons of Earth? Earth’s axis tilts different parts of Earth toward or away from the sun at different points in Earth’s orbit. 6. Why is it warmer near the Equator than the poles? It is warmer near the equator because the Earth receives th ...
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... 1. When students get to Earth, you can ask the students, “How fast does light travel?” and “How long does light take to travel from the Sun to the Earth?” Then, have students calculate the answer. Light travels at 300,000 km per second, and it takes light from the Sun 8 minutes to reach the Earth. 2 ...
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... Earth is an oblate spheroid. It is wider at the equator than at the poles. This is caused by the rotation of the Earth on its axis. The Earth’s axis is an imaginary line that runs through the center of the Earth from the north pole to the south pole. The Earth is “tilted” with relation to this imagi ...
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ScienceHelpNotes-UnitE1 - JA Williams High School

... describing the position of objects in space, using angular coordinates (e.g., describe the location of a  spot on a wall, by identifying its angle of elevation and its bearing or azimuth; describe the location of  the Sun and other stars using altitude­azimuth coordinates, also referred to as horizo ...
Exploring Our Solar System
Exploring Our Solar System

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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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