Planetary Motions - LathamWHS13-14
... http://highered.mcgrawhill.com/sites/007299181x/student_view0/chapter2/sea sons_interactive.html How long does one rotation take? How would we measure this……..? ...
... http://highered.mcgrawhill.com/sites/007299181x/student_view0/chapter2/sea sons_interactive.html How long does one rotation take? How would we measure this……..? ...
Early history of astronomy
... • The motion of a body, such as a planet or moon, along a path around some point in space • Earth's orbit is elliptical • Earth is closest to the Sun (perihelion) in January • Earth is farthest from the Sun (aphelion) in July • The plane of the ecliptic is an imaginary plane that connects Earth's or ...
... • The motion of a body, such as a planet or moon, along a path around some point in space • Earth's orbit is elliptical • Earth is closest to the Sun (perihelion) in January • Earth is farthest from the Sun (aphelion) in July • The plane of the ecliptic is an imaginary plane that connects Earth's or ...
Solar System Sort and Scale
... To recognise the distances between planets are not the same and are massive. ...
... To recognise the distances between planets are not the same and are massive. ...
The Earth in Space
... We are about 93,000,000 miles from the sun (it takes 8 minutes for sunlight to reach us!) ...
... We are about 93,000,000 miles from the sun (it takes 8 minutes for sunlight to reach us!) ...
Sun: The Nearest Star
... be for 4.6 billion years and has enough fuel to go on for another five billion years or so. At the end of its life, the Sun will start to fuse helium into heavier elements and swell to form a red giant. After a billion years as a red giant, it will suddenly collapse into a white dwarf. It may take a ...
... be for 4.6 billion years and has enough fuel to go on for another five billion years or so. At the end of its life, the Sun will start to fuse helium into heavier elements and swell to form a red giant. After a billion years as a red giant, it will suddenly collapse into a white dwarf. It may take a ...
Right Ascension / Declination
... Sirius. (We do not recommend trying this. There are much better things to be doing with your time.) There is only one slight hitch with all of this. Due to precession, the earth wobbles and in the process causes the vernal equinox to slowly move through the celestial sphere. So what we are basically ...
... Sirius. (We do not recommend trying this. There are much better things to be doing with your time.) There is only one slight hitch with all of this. Due to precession, the earth wobbles and in the process causes the vernal equinox to slowly move through the celestial sphere. So what we are basically ...
Seasons On Earth Notes
... • For 1,000’s of years astronomers have noticed the Sun gradually changes its apparent position in the sky over the course of the year. It seems to move about 1 degree each day. ...
... • For 1,000’s of years astronomers have noticed the Sun gradually changes its apparent position in the sky over the course of the year. It seems to move about 1 degree each day. ...
3observing3s
... Can measure distance on the sky in degrees (360 degrees = complete circle) Horizon -Zenith -Meridian -- line running from north to south through zenith ...
... Can measure distance on the sky in degrees (360 degrees = complete circle) Horizon -Zenith -Meridian -- line running from north to south through zenith ...
Document
... • Every celestial object Sun, Moon, planets, stars appears to circle the Earth in ONE DAY ...
... • Every celestial object Sun, Moon, planets, stars appears to circle the Earth in ONE DAY ...
HW8 - UCSB Physics
... Using this let us first calculate the three requested figures. The given mass of the earth, the sun, and the black hole of NGC 4261 are 5.97 ×1024 kg, 1.99 ×1030 kg (1 M ), and 1.2 ×109 M , respectively. Direct substitution into the equation above gives the values (a),(b),(c) for the earth, the su ...
... Using this let us first calculate the three requested figures. The given mass of the earth, the sun, and the black hole of NGC 4261 are 5.97 ×1024 kg, 1.99 ×1030 kg (1 M ), and 1.2 ×109 M , respectively. Direct substitution into the equation above gives the values (a),(b),(c) for the earth, the su ...
Our SOlar System
... 2) If the Earth was in motion around the sun, why didn't it leave behind the birds flying in the air? ...
... 2) If the Earth was in motion around the sun, why didn't it leave behind the birds flying in the air? ...
8th_Qtr2_Science_Key
... 15. The tendency of an object to continue doing what it is doing is known as: Velocity Gravity Inertia Friction 16. The motion of Earth spinning on its access is known as: Motion Rotation Revolution Radiation 17. Axis is defined as: The imaginary line that passes through the center ...
... 15. The tendency of an object to continue doing what it is doing is known as: Velocity Gravity Inertia Friction 16. The motion of Earth spinning on its access is known as: Motion Rotation Revolution Radiation 17. Axis is defined as: The imaginary line that passes through the center ...
The Sun as We See It Lecture 10, September 17, 2003
... The Sun has a “heartbeat”; its properties change on a period of 11 years ...
... The Sun has a “heartbeat”; its properties change on a period of 11 years ...
1 Astronomical Fundamentals of Time
... The fact that the ecliptic is inclined at 23.5◦ with respect to the celestial equator means that this eastward daily motion changed through the year. It is a maximum at the time of the solstices, and a minimum at the time of the equinoxes (see Figure in slides and pictures). 2. Nonuniform Motion of ...
... The fact that the ecliptic is inclined at 23.5◦ with respect to the celestial equator means that this eastward daily motion changed through the year. It is a maximum at the time of the solstices, and a minimum at the time of the equinoxes (see Figure in slides and pictures). 2. Nonuniform Motion of ...
LAB1_1SEP09
... elliptical orbit of the Earth around the sun, the sun is not directly south at local solar noon. The Earth is closest (perihelion) in late December/early January. ...
... elliptical orbit of the Earth around the sun, the sun is not directly south at local solar noon. The Earth is closest (perihelion) in late December/early January. ...
null
... At closest approach, dr /dφ = 0; light ray so rc is the solution of this equation closest b = impact r4/b2 − r2 + rs r = 0. approach parameter x Because rs is small, rc ≈ b − rs /2. We’ll need rc ≦ R☉ ; rc = R☉ is called “grazing ...
... At closest approach, dr /dφ = 0; light ray so rc is the solution of this equation closest b = impact r4/b2 − r2 + rs r = 0. approach parameter x Because rs is small, rc ≈ b − rs /2. We’ll need rc ≦ R☉ ; rc = R☉ is called “grazing ...
Orbital Geometry Notes
... • Kepler's first law: the orbits of the planets around the sun are ellipses, with the Sun at one of the foci. • The eccentricity of an ellipse can be thought of as the degree of nonroundness, or ovalness, of the orbit. ...
... • Kepler's first law: the orbits of the planets around the sun are ellipses, with the Sun at one of the foci. • The eccentricity of an ellipse can be thought of as the degree of nonroundness, or ovalness, of the orbit. ...
Homework #1
... the size of the Earth. He made a very simple model for this that involved the following assumptions: 1. The Earth is a sphere. 2. The Sun is very far away. Eratosthenes knew that at noon on June 21 (the summer solstice - longest day), the Sun would shine into the bottom of a deep vertical pit in the ...
... the size of the Earth. He made a very simple model for this that involved the following assumptions: 1. The Earth is a sphere. 2. The Sun is very far away. Eratosthenes knew that at noon on June 21 (the summer solstice - longest day), the Sun would shine into the bottom of a deep vertical pit in the ...
The solar system: The sun and the planets
... The Solar System: The Sun and the Planets Section 8.3 Pages 313-317 In orbit around the Sun, there are ________ planets and their __________, and billions of other smaller celestial objects. Name the planets from closest to farthest from the Sun. ...
... The Solar System: The Sun and the Planets Section 8.3 Pages 313-317 In orbit around the Sun, there are ________ planets and their __________, and billions of other smaller celestial objects. Name the planets from closest to farthest from the Sun. ...
Answer ALL questions from SECTION A and TWO questions from
... when hydrostatic equilibrium is established to arrival on the main sequence. Your account should describe the structure and the resulting evolutionary tracks of protostars during contraction to the main sequence. Discuss why observations of circumstellar disks, stellar winds and accretion shocks ass ...
... when hydrostatic equilibrium is established to arrival on the main sequence. Your account should describe the structure and the resulting evolutionary tracks of protostars during contraction to the main sequence. Discuss why observations of circumstellar disks, stellar winds and accretion shocks ass ...
5.1-The process of Science - Homework
... about its own axis. The sidereal day is defined as the time required for the earth to make one complete revolution in an absolute coordinate system, that is, with respect to the stars. The day in common use is the mean solar day, derived, by means of the equation of time, from the apparent solar day ...
... about its own axis. The sidereal day is defined as the time required for the earth to make one complete revolution in an absolute coordinate system, that is, with respect to the stars. The day in common use is the mean solar day, derived, by means of the equation of time, from the apparent solar day ...
Lab 4: Planetary Motions
... • Add 365 days to DOY after each year has passed • The period for Mars will be is in between the measurements, so you might not see the exact angle repeat. Need to interpolate! – Guess the DOY of Sun where period would repeat Use fractions or graph it ...
... • Add 365 days to DOY after each year has passed • The period for Mars will be is in between the measurements, so you might not see the exact angle repeat. Need to interpolate! – Guess the DOY of Sun where period would repeat Use fractions or graph it ...
Seasonal Motion
... How do we “see” that the earth is moving around the sun or v.v.? • Small discrepancy between sun’s motion and motion of stars • Sidereal vs solar day • At noon, say, the sun is not exactly in front of the same stars on the next day. – It is exactly in the south – The stars are faster, so a little w ...
... How do we “see” that the earth is moving around the sun or v.v.? • Small discrepancy between sun’s motion and motion of stars • Sidereal vs solar day • At noon, say, the sun is not exactly in front of the same stars on the next day. – It is exactly in the south – The stars are faster, so a little w ...
Planets and the Sun How Do We Size Up?
... • In order to determine size, we need a point of reference • A jet flying in the sky appears to be small due to distance, on the ground, it is very big • How does the Earth compare in size to the rest of the solar system? ...
... • In order to determine size, we need a point of reference • A jet flying in the sky appears to be small due to distance, on the ground, it is very big • How does the Earth compare in size to the rest of the solar system? ...
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.