Lab 9_ Atmospheric Retention CBuckland Report

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Sam Houston State University *

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1404

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Astronomy

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Dec 6, 2023

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docx

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Carissa Buckland PHYS 1404 14 Lab 9 Atmospheric Retention Lab 9: Atmospheric Retention The purpose of Lab 9: Atmospheric Retention is to explore various elements that play a role in the loss or retention of an atmosphere by a planet. Utilizing software and simulations from the Nebraska Astronomy Applet Project (NAAP), students will determine the escape velocities of celestial objects, understand that a primary element of atmospheric loss is from gas particles reaching escape velocity, realize that atmospheric loss is a long process and that escape only occurs for a very minute percentage of the atmosphere, and demonstrate the relationship between temperature and mass for the Maxwell distribution of atmospheric gases. Students should also display competencies in utilizing, discerning, and applying computer models, applications, and simulations, as well as communicate using vocabulary related to astronomy and atmospheric retention. Escape velocity is the lowest velocity a body must have to escape the gravitational attraction of a planet, moon, star, or other celestial body. The escape velocity of Earth is 11.2 kilometers per second. Escape velocity is directly related to the mass and radius of a planet, moon, star, or other celestial body. For gases, temperature represents the average kinetic energy contained within the molecules. All particles within a gas do not move at the same speed but instead have a distribution of speeds. The temperature of a gas significantly impacts this distribution of speeds. Higher-temperature gases are moving at faster speeds, and lower- temperature gases are moving at slower speeds. In terms of atmospheric loss, if a gas particle is moving with enough speed to exceed escape velocity and moving away from a celestial body’s surface, it can escape into space. Low escape velocities mean that gasses will escape more quickly than with high escape velocities. Atmospheric Retention begins with utilizing NAAP’s Projectile Motion Simulator to determine the escape velocity of celestial bodies. Planetary mass and planetary radius are given, initial projectile speed is estimated, the simulation is enacted, and the resulting values are observed. Once escape velocity has been found, the value can be verified using the v esc formula. The

Carissa Buckland PHYS 1404 14 Lab 9 Atmospheric Retention second portion of Atmospheric Retention uses NAAP’s Gas Retention Simulator. Students are required to add various gases, adjust the temperature, and escape velocity. Once specific gases are added, temperatures are adjusted, and escape velocity has been set, data regarding the most probable velocity can be observed. After initial observations are completed and recorded, students are asked to manipulate the temperature and escape velocity values while allowing gases to escape the chamber. The simulation is enacted, and data is collected regarding the speed at which gases exit the chamber. In the third portion of Atmospheric Retention, students are tasked with using NAAP’s Gas Retention Plot to observe retention plots for various gases, gas giants of the solar system, and icy bodies and moons of the solar system. Students then use observations made and data recorded to answer a series of questions regarding the atmospheric retention plot. In conclusion, after the completion of Atmospheric Retention, students should have a firmer grasp of the concepts that play a role in the loss or retention of atmospheric gases, as well as the ability to interpret and infer data from numerous simulations provided by NAAP.

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