- 73 Views
- Uploaded on
- Presentation posted in: General

A100 Solar System

Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author.While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server.

- - - - - - - - - - - - - - - - - - - - - - - - - - E N D - - - - - - - - - - - - - - - - - - - - - - - - - -

A100 Solar System

- Review Chapter 1, Kepler’s Laws
- Read Chapter 2: Gravity & Motion
- 2nd Homework due Sept. 26
- Rooftop Session Tuesday evening, 9PM
- Kirkwood Obs. open Wednesday Eve., 8:30-10:30
- IN-CLASS QUIZ ON WEDNESDAY!!

Today’sAPOD

The Sun Today

11:44 AM EDT

today

Dr. Phil Plait (Sonoma St. U.) acting as the Bad Astronomer balanced three raw eggs on end in late October 1998

http://apod.nasa.gov/apod/ap030923.html

- In a simple geocentric model (with the Earth at the center), planets should drift steadily eastward through the sky against the background of stars
- But sometimes, the motion of the planets against the background stars reverses, and the planets move toward the west against the background stars

- Ptolemy accounted for retrograde motion by assuming each planet moved on a small circle, which in turn had its center move on a much larger circle centered on the Earth
- The small circles were called epicycles and were incorporated so as to explain retrograde motion

Epicycles did pretty well at predicting planetary motion, but…

Discrepancies remained

Very complex Ptolemaic models were needed to account for observations

More precise data became available from Tycho Brahe in the 1500s

Epicycles could not account for observations

- Could not reconcile Brahe’s measurements of the position of the planets with Ptolemy’s geocentric model
- Reconsidered Aristarchus’s heliocentric model with the Sun at the center of the solar system

Nicolaus Copernicus (1473-1543)

- Explain retrograde motion as a natural consequence of two planets (one being the Earth) passing each other
- Copernicus could also derive the relative distances of the planets from the Sun

- Could not predict planet positions any more accurately than the model of Ptolemy
- Could not explain lack of parallax motion of stars
- Conflicted with Aristotelian “common sense”

Using Tycho’s precise observations of the position of Mars in the sky, Kepler showed the orbit to be an ellipse, not a perfect circle

Three laws of planetary motion

- Planets move in elliptical orbits with the Sun at one focus of the ellipse
- Words to remember
- Focus vs. Center
- Semi-major axis
- Semi-minor axis
- Perihelion, aphelion
- Eccentricity

- Planets orbit the Sun in ellipses, with the Sun at one focus
- The eccentricity of the ellipse, e, tells you how elongated it is
- e=0 is a circle, e<1 for all ellipses

e=0.02 e=0.4e=0.7

Which orbit is closest to a circle?

- Planets don’t move at constant speeds
- The closer a planet is to the Sun, the faster it moves
- A planet’s orbital speed varies in such a way that a line joining the Sun and the planet will sweep out an equal area each month
- Each month gets an equal slice of the orbital pie

Kepler’s 2nd Law:

Same Areas

If the planet sweeps out equal areas in equal times, does it travel faster or slower when far from the Sun?

- The amount of time a planet takes to orbit the Sun is mathematically related to the size of its orbit
- The square of the period, P, is proportional to the cube of the semimajor axis, a

P2 = a3

- Third law can be used to determine the semimajor axis, a, if the period, P, is known, a measurement that is not difficult to make

- Express the period in years
- Express the semi-major axis in AU

P2 = a3

- Express the period in years
- Express the semi-major axis in AU

For Earth:

P = 1 year, P2 = 1.0

a = 1 AU, a3 = 1.0

P2 = a3

For Mercury:

P = 0.2409 years

P2 = 5.8 x 10-2

a = 0.387 AU

a3 = 5.8 x 10-2

P2 = a3

- Express the period in years
- Express the semi-major axis in AU

For Venus:

P = 0.6152 years

P2 = 3.785 x 10-1

What is the

semi-major axis

of Venus?

P2 = a3

a = 0.723 AU

- Express the period in years
- Express the semi-major axis in AU

For Pluto:

P = 248 years

P2 = 6.15 x 104

What is the

semi-major axis

of Pluto?

P2 = a3

a = 39.5 AU

- Express the period in years
- Express the semi-major axis in AU

The Asteroid

Pilachowski (1999 ES5):

P = 4.11 years

What is the semi-major axis

of Pilachowski?

P2 = a3

a = ??? AU

- Express the period in years
- Express the semi-major axis in AU

- Express the period in years
- Express the semi-major axis in AU

- The importance of observations!
- When theory does not explain measurements, a new hypothesis must be developed; this may require a whole new model (a way of thinking about something)
- Why was the geocentric view abandoned?
- What experiments verified the heliocentric view?

ASSIGNMENTSthis week

- Review Chapter 1, Kepler’s Laws
- Read Chapter 2: Gravity & Motion
- 2nd Homework due Sept. 26
- Rooftop Session Tuesday evening, 9PM
- Kirkwood Obs. open Wednesday Eve., 8:30-10:30
- IN-CLASS QUIZ ON WEDNESDAY!!