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Ground Transportation System Design

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Ground Transportation System Design Critical Design Review February 20th, 2018 1 Overview “In Project Future Mars we will define the essential needs of a martian society of 10,000 people that will be truly self-sustaining—in other words, a colony that can live on to the distant future without any assistance from the Earth.” Analyzing the steady state solution to this problem, not how to initially establish the city. 2 Science Support CDR Presented By: Brandon Smith Science Support Group: JD Bensman, Nick Dwyer, Alaina Glidden, Henry Heim, Logan Kirsch, Annie Ping, Matt Prymek, Michael Rose, Trevor Waldman, Riley Viveros, Megan Harwell, Nick Jancich, Brandon Smith 2/20/2018 1/28/2018 3 Goals/Missions for Science Support 1. Select a lava tube for our colony 2. Identify possible landing/launch sites for the colony 3. Search for signs of past life on Mars 4. Study Martian impact craters to increase our understanding of them 5. Perform Seismography on the Mars 6. Answer longstanding questions about Phobos 7. Create a geologic history of Mars 8. Study the periodic Martian Methane 1/28/2018 4 Lava Tube Selection - Hellas Basin Requirements AG [4] -The current volume needed: 0.003 km3. (Food, City) -Nearby to resources: water glaciers (blue dots in lower image) and metal bearing clays (blue dots in upper image). -Average terrain: < 30o gradient. -Scientific Interest: impact cratering, Noachian aged geology, and 1.5 km biosignatures. - Our tube is located near the northern rim of Hellas Basin at (89.565E, -36.718N) Other Considerations -Olympus Mons (208.983E, 22.012N) [A- 1] -Elysium Planum (Approx. 173.9E, -8.4N) [A-2] 200 km Resource Extraction THEMIS V09784003 1/28/2018 5 Launch/Landing Site (See A-3 - A-4) Launch/landing site requirements: • 5-10 km away from the city • There should be no craters within the landing ellipse or within 1 km of it. • Landing site needs to be large enough for non-piloted spacecraft (i.e. Phobos sample return) Launch Site • Launch site located 5-10 km Northeast from City (89.565E, -36.718N) • Provides close, but safe distance from city incase of failure at launch site Landing Site • Phobos Mission ellipse is centered at (88.805E, -36.687N) at 36.5 km from the city and is 105.4 km x 8.8 km • Cycler taxi ellipse is 50 m x 50 m and is centered at the same location as for the Phobos mission but is too small to be seen on the map. 6 The Search for Life Mission Goals: Search areas on Mars Areas to explore: Hellas and Valles that may contain biosignatures and Marineris. These two areas were at once search for past sights of life, as well as time interacting with water. Due to the use these areas to help our significance of water in terms of life, understanding of the past Martian searching these areas for past climates. biosignatures would be advisable. Requirements: Total Area to explore: - Rover will be able to travel along ~ 12,330,000.00 km2 different terrains Distances from city: - Rover will be able to obtain 0 - 1920 km (Hellas) samples (perform spectroscopy on 5880 - 8100 km (Valles Marineris) samples) 7 Studying Impact Craters (See A-5 - A-8) Mission Goal: Observe and sample different types of Martian craters to achieve a greater understanding of them. [A-8] Requirements: Rover(s) - can be within a 400 km radius of our lava tube - will have to traverse higher gradients - will be able to perform a small borehole operations - will be able to find and collect samples [A-7] [A-6] [A-5] Rover CAD Model Created by Logan Kirsch Borehole Sample and Drill Bit CAD Model Created by Logan Kirsch 8 Seismology on Mars (See A. - A.) Mission Goals: Using seismographs, determine if Mars has “Mars” quakes. If so, use this to map the interior of Mars. Use the seismographs to determine if Mars is still somewhat geologically active. Requirements: - Establish a seismograph network Seismograph CAD Model created by Logan Kirsch on Mars - Seismographs will be approx. 10 km away from resource extraction points 9 Studying Phobos (See A-9 - A-14) Mission Goal: Determine the origin and formation of Phobos and Deimos Requirements: - A satellite that can land on Phobos - A Hohmann transfer from Mars parking orbit to Phobos orbit - With current Draim communication set up, communication to the surface of Phobos will likely be available by at least Satellite CAD Model created by Logan Kirsch one satellite at a time - Ryan Duong - Attach to Phobos, drill into surface, return to Mars with 100 kg of samples 10 Phobos and Deimos, Cont . (See A-9 - A-14) • Scaled down raptor engine • Isp = 363.3 s • Thrust = 366.3 kN • Engine Mass = 0.27 Mg • Engine Power = 5 MW • Mission Specifications • ΔV requirement of 3.31 km/s • 1300 kg initial wet mass • 776 kg of Methalox propellant • 3.16 m3 satellite volume • 4.38 hour time of flight Hohmann transfer trajectory to Phobos created in MATLAB 11 The Geologic History of Mars (See A. - A.) Mission Goals: Using a remote controlled rover, travel to areas where we would be able to see stratigraphy of the Martian crust, and establish a detail geologic record of Mars. Rover CAD Model Created by Logan Kirsch Requirements: Areas to explore: Gale crater, - Rover to traverse across Tharsis, Valles Marineris, and different landscapes Hellas. - These areas should allow us to - Rover sample collection view stratigraphy of the Martian - Photography from rover of lithosphere, and thus allow us outcrops, stratigraphic layers to create a detail, stratified geologic time scale for Mars. 12 The Mystery of Martian Methane (See A - 24) Mission Goals: - Use a rover to travel to Gale crater - Detect and analyze the methane leakage MSL detected previously - Attempt to determine the source of Methane ~ 3150 km NE of the lava tube, Coordinates (137.758E, -5.008N) Requirements: - Rover must be able to travel across Gale crater - Rover must be able to detect methane with a spectrometer - Rover must collect photos of areas where Methane was observed 13 Appendix 14 A-1: Olympus Mons Lava Tube Analysis done by Brandon Smith - Length: 50.54 km - Width: ~ 0.60 km - Height: ~ 56 m - PROS - Near Northern Lowlands - Near Tharsis - Relative Easy to locate, with respect to Olympus Mons - CONS - Far away from minerals - No nitrates - “Young” surface so not as scientifically interesting 15 A-2: Elysium Planum Lava Tube Analysis done by Megan Harwell - Flat land north of the crater - Difficult to isolate potential lava tubes - Minerals from Gusev - Olivine, pyroxene,plagioclase, FeTi oxides (MH[1]) - High concentrations of Silica nearby - Low concentrations directly around volcanic remains, however (MH[2]) - SiO2 98%(MH[3]) - TiO2 [4] - Mg, Fe, Ca, Al leaching (MH[5]) - Opaline Silica in Colombia Hills - Structurally bonded H2O (MH[6]) 16 A-3: Launch/Landing site Assumptions Launch site • There is a flat location 5-10 km northeast from our city to have a launch site • Cost of inclination change due to specified latitude for escape velocity (taxi) is relatively small Landing site • Cycler Lander can land in a 50x50 meter ellipse with Terrain Contour Matching (TERCOM, credit: Annie Ping) and human piloting (credit: John Cleveland) • Both Cycler Lander and Phobos lander can get in correct inclination before re entry to land in correct location • CD is constant for Phobos lander reentry ellipse analysis • flight path angle = -5o at an altitude of 80 km for Phobos Lander • wind effects are ignored in calculating landing ellipse • Propulsion system on the Phobos Lander, similar to the one used on the Taxi Lander, starts retrograde thrust at around an altitude = 10 km • Span on Phobos Lander does not have a huge impact on landing ellipse (see next slide, A-#) 17 A-4: Landing site Analysis-Phobos • Basic Ballistic trajectory analysis, with a Monte Carlo Simulation of 2500 trajectories • 3-sigma ellipse (98.9% of trajectories land within the ellipse) [3] • Center of Ellipse is the targeted, optimal trajectory [3] Span S (m2) semimajor axis a (km) semiminor axis b (km) Figure 1: S = 10 m2 3 52.7 4.4 5 57.7 4.4 10 53.7 4.3 2 Figure 2: S = 3 m 18 A-5: Nearest Crater (complex) • Eastern rim is ~ 128 km from the lava tube • Coordinates: (86.561E, -36.311N) • Diameter: ~ 30 km • central peak is ~ 1 km from the lowest point on the floor 19 A-6: Second crater (simple) • Eastern rim is ~ 296 km from the lava tube • Coordinates: (83.035E, -36.629N) • Diameter: ~ 24 km • lowest point is ~ 1.2 km from rim 20 A-7: Third Crater (multi-ring) • Eastern rim is ~ 365 km from the lava tube • Coordinates: (81.340E, -36.754N) • Diameter: ~ 50 km • has two rings around the center 21 A-8: Crater Study • Observe ejecta blankets for each crater type • 90% of ejecta is within 5 radii of the center of the crater • see if there is a different distribution and/or difference in particle size with distance from the point of impact • collect some ejecta material • Observe impact melts and breccia (in crater and in ejecta blanket) • knowing the volume, distribution, and characteristics of melt can give information on the processes occurring during an impact • A more extensive study of morphological characteristics at these sites could tell of the external influences on the impacts • “These might include density, velocity, and angle of impact; strength, structure, and physical state of the target material; planet’s gravitational acceleration, atmospheric density, thermal history; and postimpact processes such as erosion, sedimentation, isostasy, and magmatism” [1] • The older the crater, the harder it is to make such observations, so age is a factor 22 A-9: Phobos Science Captured Asteroids -Reflectance spectra are bright in the visible and IR regions of the spectrum.
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