After Dark in Allenspark
... solid daylight, followed by two and a half months where the night changed from 0 to 24 hours, then three and a half months of solid night, and then another two and a half months when the days get slowly longer. Try to imagine what that would do to a climate, and to a fledgling ecosystem. Far fetched ...
... solid daylight, followed by two and a half months where the night changed from 0 to 24 hours, then three and a half months of solid night, and then another two and a half months when the days get slowly longer. Try to imagine what that would do to a climate, and to a fledgling ecosystem. Far fetched ...
Keplar`s Laws of Planetary Motion
... Keplar devised three laws which describe the motions of the planets. Keplar's First Law Bodies move around the sun in elliptical orbits, with the sun at one focus. The other focus is empty. An ellipse is basically a squashed circle. All bodies orbit in an ellipse, although some are more elliptical t ...
... Keplar devised three laws which describe the motions of the planets. Keplar's First Law Bodies move around the sun in elliptical orbits, with the sun at one focus. The other focus is empty. An ellipse is basically a squashed circle. All bodies orbit in an ellipse, although some are more elliptical t ...
Review
... Interesting things about projectiles launched from the ground • time up = time down • speeds are equal at points of equal height • shape is a parabola y=ax2+b • maximum horizontal distance is obtained at 45 degrees • complementary angles (a+b=90) give same distance ...
... Interesting things about projectiles launched from the ground • time up = time down • speeds are equal at points of equal height • shape is a parabola y=ax2+b • maximum horizontal distance is obtained at 45 degrees • complementary angles (a+b=90) give same distance ...
Seasons
... b. The apparent center of the arcs is Polaris (north star) WHY? i. Since Polaris is located above the Earth’s axis of rotation, the stars and planets seem to rotate counterclockwise around Polaris at approximately 15o per hour. WHY 15o per hour? ii. The apparent daily motion of stars, moon, and pla ...
... b. The apparent center of the arcs is Polaris (north star) WHY? i. Since Polaris is located above the Earth’s axis of rotation, the stars and planets seem to rotate counterclockwise around Polaris at approximately 15o per hour. WHY 15o per hour? ii. The apparent daily motion of stars, moon, and pla ...
Review2
... b. Range of force (i.e., distances over which it operates) c. Why gravity dominates the motion of celestial objects although it is the weakest. 2. Astronomical Instruments – collecting electromagnetic radiation a. Basic telescope design – refracting vs. reflecting telescopes, and the reasons why the ...
... b. Range of force (i.e., distances over which it operates) c. Why gravity dominates the motion of celestial objects although it is the weakest. 2. Astronomical Instruments – collecting electromagnetic radiation a. Basic telescope design – refracting vs. reflecting telescopes, and the reasons why the ...
Parent signature__________________ Test
... Study tip: rewrite using bullet points and remember how many points. Explain how the sun produces energy. 5pts The sun produces energy when hydrogen combines to form helium and energy. Inside the Sun, which is a star and the largest body in the solar system, hydrogen particles smash together to make ...
... Study tip: rewrite using bullet points and remember how many points. Explain how the sun produces energy. 5pts The sun produces energy when hydrogen combines to form helium and energy. Inside the Sun, which is a star and the largest body in the solar system, hydrogen particles smash together to make ...
Seasons
... Great Pyramid and Thuban, the closest star to the rotational axis of the earth in 4420 B.C. • Betelguese, which marked the Vernal Equinox is also aligned with the southern shaft in the King’s chamber. • And others… ...
... Great Pyramid and Thuban, the closest star to the rotational axis of the earth in 4420 B.C. • Betelguese, which marked the Vernal Equinox is also aligned with the southern shaft in the King’s chamber. • And others… ...
Solar System Distance Activity
... Solar System Distance Activity Our solar system is immense in size by normal standards. We know that planets revolve around the Sun, but we don’t often consider how far each planet is from the Sun. Astronomers use the distance from the Sun to Earth as one “astronomical unit” (AU). This activity prov ...
... Solar System Distance Activity Our solar system is immense in size by normal standards. We know that planets revolve around the Sun, but we don’t often consider how far each planet is from the Sun. Astronomers use the distance from the Sun to Earth as one “astronomical unit” (AU). This activity prov ...
The Earth in Orbit - School
... If you lived in a country on the equator describe the apparent motion of the Sun every day. Because the Earth's axis of rotation is tilted we must use a different diagram. ...
... If you lived in a country on the equator describe the apparent motion of the Sun every day. Because the Earth's axis of rotation is tilted we must use a different diagram. ...
February 6
... http://www.geographyalltheway.com/ks3_geography/maps_atlases/longitude_latitude.htm ...
... http://www.geographyalltheway.com/ks3_geography/maps_atlases/longitude_latitude.htm ...
DYNAMICAL STABILITY OF SPHERICAL STARS
... by the same factor: r = r0 (1 + x), where x is a very small number that may vary with time, but not in space. Mass conservation expressed with eq. (d.1b) demands that ρ = ρ0 (1 − 3x). We shall assume that the change is adiabatic, with a constant adiabatic exponent γ : ...
... by the same factor: r = r0 (1 + x), where x is a very small number that may vary with time, but not in space. Mass conservation expressed with eq. (d.1b) demands that ρ = ρ0 (1 − 3x). We shall assume that the change is adiabatic, with a constant adiabatic exponent γ : ...
Volcanoes and Igneous Activity Earth - Chapter 4
... line joining the planet and the sun sweeps equal areas in equal times. ...
... line joining the planet and the sun sweeps equal areas in equal times. ...
Dynamics of the Earth
... Dynamics of the Earth Time Historically, a day is a time interval between successive upper transits of a given celestial reference point. upper transit – the passage of a body across the celestial meridian moving westward hour angle – the westward angular distance of an object from the meridian; neg ...
... Dynamics of the Earth Time Historically, a day is a time interval between successive upper transits of a given celestial reference point. upper transit – the passage of a body across the celestial meridian moving westward hour angle – the westward angular distance of an object from the meridian; neg ...
Time
... • What Time Is It? Before 1884, almost every town in the world kept its own local time. There were no national or international conventions which set how time should be measured, or when the day would begin and end, or what length an hour might be. However, with the vast expansion of the railway and ...
... • What Time Is It? Before 1884, almost every town in the world kept its own local time. There were no national or international conventions which set how time should be measured, or when the day would begin and end, or what length an hour might be. However, with the vast expansion of the railway and ...
ASTR 100: Homework 1 Solutions McGaugh, Fall 2008
... c = 3 × 105 km/s. The exact number is c = 299, 792 km/s; it is OK to use either value. a) 1 light-second = (3 × 105 km/s)(1 s). The seconds cancel out (see Appendix C), so 1 light-second = 300,000 km. 1 km = 0.62 miles, so (300,000 km)(0.62 miles/km) = 186,000 miles. That’s a long way to go in one s ...
... c = 3 × 105 km/s. The exact number is c = 299, 792 km/s; it is OK to use either value. a) 1 light-second = (3 × 105 km/s)(1 s). The seconds cancel out (see Appendix C), so 1 light-second = 300,000 km. 1 km = 0.62 miles, so (300,000 km)(0.62 miles/km) = 186,000 miles. That’s a long way to go in one s ...
The Sun
... The Solar Constant. Radiation energy leaving the Sun spreads out as it travels away from the Sun. At the distance of the Earth's orbit (150,000,000 km), the rate at which solar energy is received, by a surface oriented perpendicular to the Sun's direction, is called the solar constant. The solar con ...
... The Solar Constant. Radiation energy leaving the Sun spreads out as it travels away from the Sun. At the distance of the Earth's orbit (150,000,000 km), the rate at which solar energy is received, by a surface oriented perpendicular to the Sun's direction, is called the solar constant. The solar con ...
Notes and Equations
... The planets are moving, approximately in the plane of the ecliptic, with different orbital periods. We therefore see them approximately in the direction of the ecliptic. The motion of the planets can be somewhat complicated. On the average, all the major planets move from west to east as part of the ...
... The planets are moving, approximately in the plane of the ecliptic, with different orbital periods. We therefore see them approximately in the direction of the ecliptic. The motion of the planets can be somewhat complicated. On the average, all the major planets move from west to east as part of the ...
Corresponding Angles and Distances forvJarded expressly for
... orbit; but the stars, which have latterly been gradually approaching, have within the last two years closed up so rapidly as to be in the early part of the current year quite beyond the power of my instrument, the distance being estimated as not exceeding o"· 4, while only a rough guess could be mad ...
... orbit; but the stars, which have latterly been gradually approaching, have within the last two years closed up so rapidly as to be in the early part of the current year quite beyond the power of my instrument, the distance being estimated as not exceeding o"· 4, while only a rough guess could be mad ...
a planet rotates on its own axis and revolves around
... a path Revolution- Earth completes an orbit around the sun which happens every 365.24 days or a year (leap years would be 366 days) This is how the seasons occur ...
... a path Revolution- Earth completes an orbit around the sun which happens every 365.24 days or a year (leap years would be 366 days) This is how the seasons occur ...
Solar System Bead Distance Activity
... Our Solar System is immense in size by normal standards. We think of the planets as revolving around the Sun, but rarely consider how far each planet is from the Sun. Furthermore, we fail to appreciate the even greater distances to the other stars. Astronomers use the distance from the Sun to the Ea ...
... Our Solar System is immense in size by normal standards. We think of the planets as revolving around the Sun, but rarely consider how far each planet is from the Sun. Furthermore, we fail to appreciate the even greater distances to the other stars. Astronomers use the distance from the Sun to the Ea ...
Review-Sheet-sun-solar-system-galaxies-and-cosmology-fall
... 1. What are the three layers of the sun’s interior? What part is responsible for fusion? 2. What are the three layers of the Sun’s atmosphere? Be able to describe them briefly, such as lowest layer, the visible surface, etc… 3. What is the solar wind? What happens when the solar wind gets trapped in ...
... 1. What are the three layers of the sun’s interior? What part is responsible for fusion? 2. What are the three layers of the Sun’s atmosphere? Be able to describe them briefly, such as lowest layer, the visible surface, etc… 3. What is the solar wind? What happens when the solar wind gets trapped in ...
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.