THE COLORADO MODEL SOLAR SYSTEM
... Sun. Explain why not. (Hint: If you’re having trouble answering this question, have a classmate “orbit” at Mercury’s distance of 6 meters (20 feet) from the Sun while you observe from Earth - and note which directions you look to follow Mercury’s motion.) ...
... Sun. Explain why not. (Hint: If you’re having trouble answering this question, have a classmate “orbit” at Mercury’s distance of 6 meters (20 feet) from the Sun while you observe from Earth - and note which directions you look to follow Mercury’s motion.) ...
Coronal Mass Ejection
... thermonuclear fusion of hydrogen into helium. • Gravitational and thermal equilibrium determine the Sun’s internal structure and its rate of energy generation. • The Sun’s atmosphere displays its own version of weather and climate, governed by solar magnetic fields. Solar weather has important influ ...
... thermonuclear fusion of hydrogen into helium. • Gravitational and thermal equilibrium determine the Sun’s internal structure and its rate of energy generation. • The Sun’s atmosphere displays its own version of weather and climate, governed by solar magnetic fields. Solar weather has important influ ...
Lecture03
... ellipse whose eccentricity is e = 0.017 (Appendix 1). • Because its orbit is and ellipse rather than a perfect circle, the Earth is slightly farther from the Sun in July than it is in January (Fig. 2-22). But this relatively small distance variation is not responsible for Earth’s seasons. ...
... ellipse whose eccentricity is e = 0.017 (Appendix 1). • Because its orbit is and ellipse rather than a perfect circle, the Earth is slightly farther from the Sun in July than it is in January (Fig. 2-22). But this relatively small distance variation is not responsible for Earth’s seasons. ...
ASTR 111 Lab Manual - Ohio Wesleyan University
... celestial equator, and is analogous to latitude on the surface of the Earth. Instead of appending “N” or “S” to the declination, we use the convention that objects north of the celestial equator have positive declination, while objects south of the celestial equator have negative declination. On you ...
... celestial equator, and is analogous to latitude on the surface of the Earth. Instead of appending “N” or “S” to the declination, we use the convention that objects north of the celestial equator have positive declination, while objects south of the celestial equator have negative declination. On you ...
what is your position?
... After the observation, the navigator consults a nautical almanac with the predicted lunar distances and the times at which they will occur.Through the comparison of the adjusted, observed lunar distance with the predicted value, the navigator can calculate his longitude. However, this method is not ...
... After the observation, the navigator consults a nautical almanac with the predicted lunar distances and the times at which they will occur.Through the comparison of the adjusted, observed lunar distance with the predicted value, the navigator can calculate his longitude. However, this method is not ...
Ayres-Kepler-ASC
... fast rotating stars, but also root of magnetic braking, which ultimately quenches activity. ...
... fast rotating stars, but also root of magnetic braking, which ultimately quenches activity. ...
Lecture Two (Powerpoint format)
... Cacophony in the Celestial Harmony -The Problem of Retrograde Motion The geocentric model of the universe works very well for stars, but there is a major problem for planetary motion. Occasionally, the outer planets will appear to slow down, stop, then reverse their direction on the night sky - ...
... Cacophony in the Celestial Harmony -The Problem of Retrograde Motion The geocentric model of the universe works very well for stars, but there is a major problem for planetary motion. Occasionally, the outer planets will appear to slow down, stop, then reverse their direction on the night sky - ...
Precession of the Equinoxes and its Importance in Calendar Making
... ent path of the Sun in the celestial sphere remains the same, the moon and the planets show some deviations in their motions. The moon and the planets move to some extent towards north and south of the ecliptic. This deviation for the moon does not exceed much more than 5 degrees, while the planets ...
... ent path of the Sun in the celestial sphere remains the same, the moon and the planets show some deviations in their motions. The moon and the planets move to some extent towards north and south of the ecliptic. This deviation for the moon does not exceed much more than 5 degrees, while the planets ...
Lesson 120125 - WordPress.com
... Example of how to use this Q2. The other planets called Abbott and Costello orbit another star. Abbott is 4 times further away from this star than Costello is. Costello takes 5 years to orbit the star. How long does Abbott take to orbit ? ...
... Example of how to use this Q2. The other planets called Abbott and Costello orbit another star. Abbott is 4 times further away from this star than Costello is. Costello takes 5 years to orbit the star. How long does Abbott take to orbit ? ...
Planets in the Sky
... Mars: no restrictions on distance from Sun in sky Jupiter: no restrictions on distance from Sun in sky Saturn: no restrictions on distance from Sun in sky ...
... Mars: no restrictions on distance from Sun in sky Jupiter: no restrictions on distance from Sun in sky Saturn: no restrictions on distance from Sun in sky ...
Lecture 1
... With parallax, we learned that the position of a near object relative to a distant object can change if the observer moves. With rotation, the time it takes for the position of a near object to change relative to a distant object can be different if the observer moves. ...
... With parallax, we learned that the position of a near object relative to a distant object can change if the observer moves. With rotation, the time it takes for the position of a near object to change relative to a distant object can be different if the observer moves. ...
29-1
... _____ 18. What is the speed of light? a. 300,000 km/hr b. 300,000 km/s c. 300,000 m/hr d. 300,000 m/s 19. How much mass is changed into energy in the sun every second? ____________________________________________________________ THE SUN’S INTERIOR ...
... _____ 18. What is the speed of light? a. 300,000 km/hr b. 300,000 km/s c. 300,000 m/hr d. 300,000 m/s 19. How much mass is changed into energy in the sun every second? ____________________________________________________________ THE SUN’S INTERIOR ...
CHAPTER 1
... 2. The planets lack the simple, uniform motion of the Sun and Moon. They sometimes stop their eastward motion among the stars and move westward for a while. This is called retrograde motion. 3. The planets always stay near the ecliptic. In addition, Mercury and Venus never appear very far from the p ...
... 2. The planets lack the simple, uniform motion of the Sun and Moon. They sometimes stop their eastward motion among the stars and move westward for a while. This is called retrograde motion. 3. The planets always stay near the ecliptic. In addition, Mercury and Venus never appear very far from the p ...
CHAPTER 5,Planetary Orbits
... A.M. or P.M. in the above equation; use a 24 hour clock only. If the Sun, planet, or Moon is not near the celestial equator, the above equation may be off by more than an hour. The farther away one or both objects are from the celestial equator, the larger the error. The value of the equation of tim ...
... A.M. or P.M. in the above equation; use a 24 hour clock only. If the Sun, planet, or Moon is not near the celestial equator, the above equation may be off by more than an hour. The farther away one or both objects are from the celestial equator, the larger the error. The value of the equation of tim ...
Introduction to Astronomy (high school)
... the beginning of the season of autumn (fall) on our calendar. On those two days of the year, the Sun will rise in the exact east direction, follow an arc right along the celestial equator and set in the exact west direction. ...
... the beginning of the season of autumn (fall) on our calendar. On those two days of the year, the Sun will rise in the exact east direction, follow an arc right along the celestial equator and set in the exact west direction. ...
C:\Documents and Settings\Administrator\Desktop\Lecture 15.wpd
... The Central Problem in astronomy is distance. What we see is basically a twodimensional picture of the sky. To interpret many pieces of information available to the astronomer we need to know how far away a star or galaxy is. Example: If you look at the sky, Sirius is brighter than Betelgeuse. But B ...
... The Central Problem in astronomy is distance. What we see is basically a twodimensional picture of the sky. To interpret many pieces of information available to the astronomer we need to know how far away a star or galaxy is. Example: If you look at the sky, Sirius is brighter than Betelgeuse. But B ...
Making an ellipse
... A comet is an icy small Solar System body that, when passing close to the Sun, heats up and begins to outgas, displaying a visible atmosphere or coma, and sometimes also a tail. These phenomena are due to the effects of solar radiation and the solar wind upon the nucleus of the comet. ...
... A comet is an icy small Solar System body that, when passing close to the Sun, heats up and begins to outgas, displaying a visible atmosphere or coma, and sometimes also a tail. These phenomena are due to the effects of solar radiation and the solar wind upon the nucleus of the comet. ...
Earth & Space - Stars - Students, Teachers and Resources
... • Moves with the seasons north and south of the equator between the Tropics of Cancer and Capricorn • Close to the equator, the ITCZ influences the weather twice a year during the equinoxes in March and September. • Near the Tropic of Cancer, the ITCZ approaches only during June and July, and climat ...
... • Moves with the seasons north and south of the equator between the Tropics of Cancer and Capricorn • Close to the equator, the ITCZ influences the weather twice a year during the equinoxes in March and September. • Near the Tropic of Cancer, the ITCZ approaches only during June and July, and climat ...
naap_motion1_sg
... Dragging the stick figure allows one to very conveniently change latitude. Dragging the stick figure on top of the subsolar point effectively puts the observer at the latitude where the direct rays of the sun are hitting. ...
... Dragging the stick figure allows one to very conveniently change latitude. Dragging the stick figure on top of the subsolar point effectively puts the observer at the latitude where the direct rays of the sun are hitting. ...
Latitude and Longitude - Northside Middle School
... lines connect the North Pole with the South Pole The line of 0° longitude is the Prime Meridian Longitude lines give directions East or West of the Prime Meridian There are 180° of longitude East or West of the ...
... lines connect the North Pole with the South Pole The line of 0° longitude is the Prime Meridian Longitude lines give directions East or West of the Prime Meridian There are 180° of longitude East or West of the ...
Earth Science Chap.2 Sect. 2
... As the earth rotates about its axis, the direction in which the axis points slowly changes in relation to distant stars. The axis has not always pointed toward the North Star and will not in the distant future. Precession: a circular motion of the earth’s axis which causes the change relative to dis ...
... As the earth rotates about its axis, the direction in which the axis points slowly changes in relation to distant stars. The axis has not always pointed toward the North Star and will not in the distant future. Precession: a circular motion of the earth’s axis which causes the change relative to dis ...
zenith - Gardner-Webb University
... Shadow plot B Shadow plot C More than one of the plots are possible, on different days of the year. None of the plots are possible. ...
... Shadow plot B Shadow plot C More than one of the plots are possible, on different days of the year. None of the plots are possible. ...
Quiz # 10
... 2. The hotter region directly above the Sun's visible surface is called the a. chromosphere b. photosphere c. corona d. ionization region e. convection zone 3. The ten million tons of particles that escape the Sun each year in the form of the solar wind get out mainly from regions called a. sunspots ...
... 2. The hotter region directly above the Sun's visible surface is called the a. chromosphere b. photosphere c. corona d. ionization region e. convection zone 3. The ten million tons of particles that escape the Sun each year in the form of the solar wind get out mainly from regions called a. sunspots ...
The Celestial Sphere
... circle every 24 hours… “Diurnal Motion” Except the points directly above the north and south poles which do not appear to move. The sphere spins around them. They are called the North and South Celestial Poles. Half-way between the poles, above the Equator, lies the Celestial Equator it spins the mo ...
... circle every 24 hours… “Diurnal Motion” Except the points directly above the north and south poles which do not appear to move. The sphere spins around them. They are called the North and South Celestial Poles. Half-way between the poles, above the Equator, lies the Celestial Equator it spins the mo ...
Equation of time
The equation of time describes the discrepancy between two kinds of solar time. These are apparent solar time, which directly tracks the motion of the sun, and mean solar time, which tracks a fictitious ""mean"" sun with noons 24 hours apart. Apparent (or true) solar time can be obtained by measurement of the current position (hour angle) of the Sun, or indicated (with limited accuracy) by a sundial. Mean solar time, for the same place, would be the time indicated by a steady clock set so that over the year its differences from apparent solar time average to zero.The equation of time is the east or west component of the analemma, a curve representing the angular offset of the Sun from its mean position on the celestial sphere as viewed from Earth. The equation of time values for each day of the year, compiled by astronomical observatories, were widely listed in almanacs and ephemerides.