Embedded Files
Task Overview
Task Overview
Task: Use the formulas from Kepler's Laws to determine the specifications for the eccentricity of the orbit of a planetary object
Use mathematical or computational representations to predict the motion of orbiting objects in the solar system and then rationalize how changes in an orbit can affect surface conditions and/or processes on a planetary object
First law— e = c/a
Second law— equal area in equal time
Third law— T^2 ∝ a^3
However, do not come into this summative without having completed the study guide. You will not be presented with problems so simple as me providing c and a for you to then just calculate e. No, you will have to use algebraic and geometric thinking to solve for c and a, to then calculate eccentricity. Likewise, you will have to use logic and reasoning with calculated values to compare the amount of time an object spends in an orbital sector.
Assessment Criteria
Assessment Criteria
Apply ratios, rates, percentages
Make accurate calculations.
Accuracy is the degree to which a measured value is to the actual value. In other words, compute/calculate correct numbers. Show all your work (If being asked to calculate in scientific notation, show all work in scientific notation). Round all values to Sig Figs.
Use conceptual ideas to explain phenomenon
Use scientific terminology accurately in appropriate contexts. Use scientific information accurately. Organize processes or explanations logically. Do not guess what is happening or why, but use reason and logic.
Task 1, First Law
Task 1, First Law
Use the provided information of a labelled model of an ellipse to calculate the values of c and a for an object with orbital motion
Use e=c/a to determine the eccentricty of the orbiting object
Task 2, Second Law
Task 2, Second Law
Calculate the sector areas of an elliptical orbit, where the sector areas are of different areas
Use the calculated values to make a claim about the proportion of an orbital period in a given sector
Task 3, Third Law
Task 3, Third Law
Calculate the missing values relevant to the Third Law for three orbits around the same massive object
Task 4, Magnet Summary
Task 4, Magnet Summary
Use the magnet summary strategy for an informational text about orbital motion
Based on your magnet summary, make a claim about orbital motion and climate
Orbital motion
Set the eccentricity to 0, then start.
Increase the eccentricity to 0.24, then start.
Repeat this with eccentricities of 0.5, 0.74 and 0.9.
Using your new knowledge from the "uniform circular motion" exercise, make observations of how velocity and force changes as the eccentricity of orbital motion changes. Be able to calculate C, A and E in addition to understanding the structure of an ellipse.
At which point of its elliptical orbit is a planet located at a given time? In 1609, Johannes Kepler could answer this question with the following simple law: Kepler's second law of the undisturbed planetary motion: The line joining the planet to the Sun sweeps out equal areas in equal intervals of time. This law shall be illustrated by a computer simulation. READ THE INFORMATION.
The demo shows two planets in circular orbits around a star. Using the sliders, you can see how changing the radius affects the orbital period (in other words, how fast it makes the planet), in addition to changing the mass of the star.
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