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astronomy 3
| Question | Answer |
|---|---|
| How do we terraform? | Increase atmospheric pressure → increase greenhouse gases → temperature rises → permafrost melts |
| What makes Enceladus so interesting for astrobiology? | It has some liquid subsurface water that can interact with the surface and the heated, rocky seafloor |
| For tidal heating to occur, besides being close to a massive planet, what is required? | The moon has to have a slightly eccentric orbit around the planet |
| Which one is the biggest obstacle for life (as we know it) on Titan's surface? | The low temperatures |
| Why is it so difficult to directly detect exoplanets around nearby stars? | Because the faint planet is seen too close to a billion times brighter object, the star |
| Why are the radial velocity (RV) and transit (Tr) methods complementary? | The RV method measures the (minimum) mass while the Tr method measures the size (radius) of the planet |
| What was surprising about 51 Pegasi b? | 4 day orbit around Jupiter |
| What makes Europa interesting for life? | ocean is both in contact with the rocky interior and the icy surface |
| What are the prospects for life in the outer solar system? | Europa, Enceladus, Titan, and other moons |
| What is tidal heating? | Frictional heating caused by gravitational forces stretching and compressing a moon, generating internal heat |
| Is there a possibility of habitats on Europa due to chemical exchange? | Yes, chemical reactions between the ocean and rocky seafloor could produce energy rich molecules |
| Which is NOT required for tidal heating (Io & Europa)? | The strong magnetic field of Jupiter |
| Which is NOT required for life on Jovian moons? | A very dense atmosphere |
| Why is Titan interesting for astrobiology? | Its dense atmosphere contains organic molecules and it has liquids on the surface |
| Why is Enceladus interesting? | Its icy geysers indicate liquid water below the surface |
| Why is it difficult to directly image exoplanets? | The faint image of the planet is overwhelmed by the super bright image of the star |
| Why does the RV method give only minimum mass? | Because we don’t know the angle of the planet’s orbit relative to our line of sight |
| Which planet is most detectable by radial velocity? | A massive planet orbiting close to its star |
| Which planet is most detectable by transit? | A large planet orbiting close to its star |
| Two planets have same mass but different sizes—what’s true? | one must be dense-er than the other |
| Why was the Kepler telescope launched into space? | Because Earth’s atmosphere is too variable to detect small transit signals |
| Which planets did Kepler find most often? | Super Earths (1.4–2.8 Earth radii) Planets smaller than Neptune at orbital separations of < 1 AU |
| What is remarkable about the TRAPPIST-1 system? | It has seven Earth size transiting planets in a compact system |
| What are examples of biosignatures? | All of the above |
| Best way to detect life on exoplanets? | Obtaining spectra to determine atmospheric composition |
| Why are biosignatures more likely than SETI to find life first? | Because even life on Earth was microbial for most of its history |
| What type of planets were most frequently discovered by Kepler? | Planets smaller than Neptune at orbital separations of < 1 AU |
Created by:
rileyrola