Intergalactic Planetary
mission
Our mission was to create a series of models representing our solar system. In this, we created multiple different drafts. Our first being the simplest, using our previous knowledge on basic topics such as the order of which the planets are in, and our last being the most in depth which consisted of things such as escape velocity, orbital period, and gravitational force.
the process
The first assignment of this project that we were given to do was to draw out our understanding of what the solar system looks like. We then got a piece of poster paper and put the planets in order from the Sun to Neptune. After that, we drew a more accurate model overlapping it by drawing the scaled down size of each planet. Next, we took our work even farther and applied our new knowledge on space to the phenomenon that we focused on: the farther away a planet is from the sun, the longer it takes to complete an orbit around the sun and the lower the orbital velocity. Using the data that we were given, we put this into our model: v= 2 pi r/86400 t. Lastly, our final model consisted of two parts. For part one of it, we made predictions for Planet X, Planet Y, and Earth based off of the information in the table below, which we then found surface temperature, gravitational force, orbital period, and escape velocity. For part two of the model, we calculated the orbital period of Planet X and Planet Y as well as our weight if we were to be on the surface of them.
evidence of work
First Draft
This shows accurate distances between the planets.
Second Draft
This shows the data backing up our chosen phenomenon on distance from the sun and orbital period resulting in orbital velocity.
Part 1
This is our model showing the results that we were able to uncover using limited data.
Part 2
This shows our weight on Planet X and Planet Y as well as our weight on them.
content
Universal Law of Gravitation: Every point of mass attracts every other point of mass which is directly proportional to the sum of their mass and indirectly proportional to their distances. This can be represented by the equation F= Gm1m2/d^2. We used this while solving our practice problems in the book which included gravitation.
Gravitational Force: The force of attraction between all masses in the universe. This can be represented by the equation F= Gm1m2/d^2. We used this in our model when we found our weight on the other planets.
Inverse Square Law: A physical quantity varies inversely as another quantity is squared. We used this when while solving our practice problems.
Orbital Period: The time that it takes to complete one full orbit around the sun. We used this to describe our phenomenon as well as we were able to predict it in our final model.
Distance to Sun: How far away a planet is from the sun. This is measured in meters and we were able to use this in our equation v= 2 pi r/86400 t as the radius (r).
Radius of Planet: The distance between the surface of a planet and it's center. We used this in our practice problems.
Crust: The outer layer of a planet which is made up of materials such as igneous, sedimentary, and metamorphic rocks.
Mantle: The layer below the crust which is made up of a rock known as lithosphere.
Liquid Outer Core: A fluid layer above the Earth's solid inner core that 1,500 miles thick. It is made of iron and nickel.
Solid Inner Core: The center of the Earth. The Earth's solid inner core has a radius of 760 miles and is made up of iron-nickel alloy.
Orbital Velocity: The velocity that an object moves around another object. This is measured in meters per second.
Rotation: The spinning motion that takes place when an objects circles around it's center of mass. We included this during our discussion and lab where we used flashlights to show the Sun's effect on the Earth (seasons, night and day, etc).
reflection
This project was more challenging for me since we weren't able to see a physical model of how everything works and it was less hands on but, it did give me a better chance to focus on learning how to do the calculations better. Because of this, I personally think it will allow me to be a little bit more confident going into other projects were calculations are more dominant. Although, collaboration was hard at times since one of my teammates was always either getting our group off task or wouldn't stay with our group at all, providing little help. Other than that, this project not only gave me more insight on our solar system and space itself, but it also gave me support and experience for future projects.