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EAS 206 > Imaads > Flashcards

Imaads Flashcards

1
Q

What is a planet?

A

Cold object that orbita around a central luminous start

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2
Q

What is a Planetary body?

A

General term for any body orbiting a star includes planets and their natural satellites/moons

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3
Q

Terrestrial (Inner) planets

A

Relatively small, rocky (“Earth-like”) bodies closest to the sun
↳ moon is studied as a terrestrial planet

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4
Q

General planet info

A
  • Mercury
    ↳ larger than earths moon & closes to sun
  • Venus
    ↳ 2nd closest planet & shrouded by clouds
    ↳ lots of craters and mountain belts
  • Earth
    ↳ lots of plate tectonics, erosion, has life along with atmosphere
  • Moon
    ↳ orbits earth
  • Mars
    ↳ very thin atmosphere
    ↳ erosion by water, lots of volcanoes & valleys
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5
Q

Asteroid

A

small rocky or metal-rich planetary body orbiting the sun

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6
Q

Asteroid belt

A
  • region between the orbits of Mars and Jupiter where most asteroids are found
  • asteroids range from 1 - 1000km in diamerter
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7
Q

Gas Giants (outer Planets)

A

Large planets that have a deep atmosphere and no solid surfaces
↳ icy/rocky

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8
Q

Comets

A

small, ice rich bodies which formed at the outer edges of the solar system

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9
Q

Neptune & Uranus

A
  • Both are gas and ice rich
  • Have icy moons
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10
Q

The three main tock types

A

Igneous, Sedimentary, and Metamorphic

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11
Q

Law of Superposition?

A

Each layer of sediment is older than the layer above it and younger than the layer below it

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12
Q

Law of Cross-cutting Relationships?

A

If a fault or other body of rock cuts through another body of rock then it must be younger in age than the rock through which it cuts

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13
Q

Law of Inclusions?

A

One rock included in another is older than the rock that includes it

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14
Q

Law of original horizontality

A

Sedimentary layers are deposited horizontally

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15
Q

Crust

A

The outermost layer, on top of the mantle

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16
Q

Mantle

A

It has upper and lower sections and includes the asthenosphere, iron, and magnesium-rich silicate minerals

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17
Q

Asthenosphere

A

The top part of the upper mantle where it is plastic, and partly molten

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18
Q

Lithosphere

A

includes the rigid part of the mantle and the overlying crust, rides on the plastic asthenosphere

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19
Q

The three ways we know what the interior of the Earth looks like

A

Density, Seismic data, Meteorites

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20
Q

Main geologic processes active on Earth today

A

Tectonics, volcanic activity, mass wasting, water, wind, ice -> erosion and deposition of sediment, impact crater, life

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21
Q

Fusion

A

The combination of two or more nuclei to form a different, heavier, element; the by-product is radiation

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22
Q

What Keeps a Star together?

A
  • Gravity attempts to make the star collapse
  • High gas pressure opposes gravity
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23
Q

Supernova

A

The cataclysmic explosion of a star, as a result of internal nuclear reactions

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24
Q

Nebula

A

Dust in space with a density of 1,000 gas molecules/10cm^3

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25
Q

Gravitational Collapse

A

When molecules are concentrated, attracted to each other; may be triggered by a nearby supernova

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26
Q

T Tauri stars

A

stars that are similar in mass to the
Sun, but only about 1 million years old

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27
Q

Proplyds

A

disks of dust and gas around young
stars; contraction of “protoplanetary disks”

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28
Q

Meteorites

A

extraterrestrial rock that’s fallen through our atmosphere

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29
Q

Refractory

A

materials that form solids at
very high temperatures

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30
Q

Volatile

A

materials that condense/solidify
at very low temperatures

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31
Q

Planetesimal

A

Small solid bodies, ~100km across, that formed from grain-to-grain accretion of dust

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32
Q

Accretion

A

Solids come together to form larger objects through gravitational attraction and collisions

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33
Q

Differentiation

A

The separation of materials in a planetary body according to density and chemical affinity

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34
Q

Conduction

A

The vibrational energy of an atom is transferred to adjacent atoms

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35
Q

Convection

A

Warm material expands and moves upwards, displacing cooler, denser materials downwards

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36
Q

Radiation

A

The emission of electromagnetic waves from a hot body’s surface to its surroundings

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37
Q

Law of Cross-cutting Relationships for impact cratering

A

If an impact crater, fault, or body of rock cuts through another body of rock then it must be younger than the rock through which it cuts

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38
Q

Three things that must be explained by any model for how the solar system was formed

A
  • The planets orbit in the same plane
  • They orbit the Sun in the same direction
  • The Solar System is zoned from rocky inner planets to gas-rich outer planets to ice-rich comets
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39
Q

Why the Moon always shows the same side to the Earth

A

The period of rotation and period of revolution are exactly the same

40
Q

Two surfaces on the Moon that can be easily seen from Earth

A
  • Maria (smooth surfaces)
  • Terrae (cratered highland)
41
Q

Crater sizes on the moon

A
  • 20 to 200km diam
    ↳ have central peaks
  • crater > 300km diam
    ↳ called multi ring basins & spacing of rings increases outward
42
Q

What is KREEP

A

KREEP is a component found in soils, breccias and impact melts

43
Q

Fire fountaining

A

Volcanic activity on the Moon, it creates Lunar Glass Beads

44
Q

Anorthosite

A

Most abundant and
oldest rock type

45
Q

Breccia

A

A rock made up of
angular fragments of
other rocks
↳ more basalts

46
Q

Regolith

A
  • Mixture of rock fragments
  • Formed during micrometeorite impacts;
47
Q

Explain why mare basalts can flow such great distances on the Moon

A

They contain more iron and less silicate and aluminum, which causes lunar basalts to have a lower viscosity

48
Q

List the main observations that any model for the formation of the Moon must explain

A
  • size of the moon relative to earth
  • The low bulk density/size of its iron core and its composition
  • Moon has little water and is depleted in other elements
  • it’s orbit
49
Q

Giant Impact Hypothesis

A
  • The giant impact hypothesis proposes that the Moon formed from debris ejected during a collision between the early Earth and a Mars-sized protoplanet around 4.5 billion years ago.
50
Q

The major discoveries made by the Lunar Reconnaissance Orbiter mission

A

evidence of water on the Moon, Moon caves, map of the lunar south poles, more topography, temperature map

51
Q

Describe how the crystallization of a magma ocean explains the anorthosite composition of the Moon’s crust

A
  • pyroxene and olivine in the magma sink and the anorthosite (lighter mineral) floats
52
Q

Explain how the lunar cratering record is used to date the surfaces of other planets

A
  • the number of craters on a part of a planetary surface can be used to estimate its age; the more craters, the older the age
53
Q

Explain how it is possible that water ice could be present on Mercury’s surface

A

There are some deep craters at the poles of Mercury that are permanently shadowed which protect/preserve any volatiles present in the craters

54
Q

Describe Mercury in terms of its orbit, length of the day, and length of the year

A

Orbit: ~1/3 of the distance from the Sun to Earth
Length of the Day: 59 earth days
Length of the Year: 88 Earth Days

55
Q

Describe the surface of Venus as seen from landersDescribe the surface of Venus as seen from landers

A

It has a very rough, rocky surface and due to the atmosphere, everything has a yellow tintIt has a very rough, rocky surface and due to the atmosphere, everything has a yellow tint

56
Q

Mercury’s unique tectonic features

A

Compressional stresses are dominant. Mercury has contracted 7 km in radius

57
Q

What are Lowlands, Uplands and Highlands

A
  • Lowland: below 0km of elevation
  • Uplands: around 0-2km of elevation (isolated domes)
  • Highlands: areas that are > 2km (mountain regions)
58
Q

Tectonic features of Venus:
What do fracture belts, domes and rifts represent on Venus

A

Extension

59
Q

Tectonic features of Venus:
What do mountain and ridge belts represent on Venus

A

Compression

60
Q

What are Coronae?

A
  • Volcano-tectonic features that unique to Venus
  • Corona: system of concentric fractures and ridges surrounding a central plain
    (STAGES ARE NOT IMPORTANT WE WERE TESTED ALR)
61
Q

Atmosphere of Venus

A

Effects:
- High surface temps (greenhouse effect)
- Wind erosion and deposition

62
Q

How does the greenhouse effect affect venus?

A
  • It is too hot for liquid water to condense, water stays as a gas, CO2 stays as a gas
  • TLDR for “runaway greenhouse effect”: it’s super hot because of all the CO2 and you need to cool the atmosphere a bunch to stabilize all the carbonate
63
Q

Geologic History of Mars: Pre-Noachian

A
  • Pre-Noachian
    ↳ Magma formation
    ↳ large basin formation from impacts
64
Q

Geologic History of Mars: Noachian

A
  • Noachian
    ↳ Early volcanism
    ↳ Tectonism begins
65
Q

Geologic History of Mars: Herperian

A
  • Herperian
    ↳ Valles Mariuneris forms
    ↳ Elysium volcanoes form
66
Q

Geologic History of Mars: Amazonian

A
  • Amazonian
    ↳ Ongoing volcanism
    ↳ Polar Icy deposits
    ↳ mass movement
67
Q

Mars Hydrological Cycle

A

The current hydrologic cycle on Mars involves the periodic release of ground ice into the atmosphere as vapour, which travels to and freezes at the poles, with pole ice sublimating in summer and travelling to the colder pole, and surface frost precipitating and sublimating due to daily temperature changes.

68
Q

Ground Ice in Mars

A
  • Right now liquid water is NOT stable at the surface of present day mars
  • Water ice is present
69
Q

Mass movement in Mars

A
  • Mass movement: gravity-driven downhill
    movement of unconsolidated material
70
Q

Slope Streak characterization

A

Slope Streak: start in a point upslope, widen downslope
- Wet (liquid water)
↳ melting of frost/ice
↳ groundwater spring
- Dry
↳ Dust avalanching

71
Q

Where do Humans appear on the tree of life?

A

Eukaryota, under Animals

72
Q

Earliest forms of life

A
  • Stromatolites: formed by filamentous bacteria mats that trap sediment as bacteria grows
73
Q

What is a Gas Giants

A

Relatively large planets that have deep atmospheres and have NO solid surfaces; have rings of particles around them, and many icy/rocky satellites

74
Q

What is Jupiter’s atmosphere made of

A
  • 90% H2 and 10% He
  • little amounts of water,methane and ammonia
  • Clouds in jupiter are made of ammonia ice
75
Q

Difference between Earth and Jupiter

A
  • Earth is composed of dense silicates while Jupiter is made up mostly of hydrogen and helium
  • Jupiters magnetic field is 20,000 times that of earth
  • Jupiter has a quicker period of rotation (9.9 hours)
  • Jupiter is also much colder than earth
76
Q

Jupiter internal structure

A
  1. Atmosphere and Molecular Hydrogen Layer - beneath the atmosphere, there is a molecular hydrogen layer that extends to about 20,000 km.
  2. Metallic Hydrogen Layer
  3. Core - Jupiter has a volatile-rich core estimated to be 10-15 times the mass of Earth
77
Q

Differences between Jupiter and Saturn

A
  1. Jupiters magnetic field is significantly stronger than Saturn (20,000 vs 0.4)
  2. They are composed of the same things in the atmosphere
  3. Jupiter is slightly warmer than Saturn
78
Q

Saturns Atmosphere

A
  • 96% H2, 3% He, small amounts of Methane & Ammonia Clouds
79
Q

Saturns internal structure

A
  • eddies and cyclones cause by heat released from the planets interior
    1. Atmosphere consists of H2 and He
    2. Molecular Hydrogen Layer: 30,000km thick composed of H2
    3. Metallic Hydrogen Layer: contains metallic H+
    4. Core: volatiles and silicates
80
Q

Uranus compared to Jupiter

A
  • Uranus has a more complex composition than jupiter
  • Significantly weaker magnetic field than jupiter
  • Almost double the period of rotation of jupiter (uranus 17.2hr)
81
Q

Uranus – Atmosphere & internal structure

A

Composition:
– 83% H2, 15% He, 2% CH4
- Internal Structure:
- rich in ice and silicates
- Core of volatiles and silicate rock

82
Q

Uranus compared to Neptune

A
  • Both have a complex bulk composition
  • Same things make up the atmosphere
  • similar magnetic fields & temps
83
Q

Neptune – Atmosphere & Internal Structure

A

Composition:
– 80% H2
– 18% He
– 1.5% CH4

  • Internal Struc: Higher density
  • Core of ice and silicate rock
84
Q

How each planet gets their heat

A
  • Jupiter, Saturn have a greater internal heat than what they get from the sun
  • Uranus receives less heat from the Sun and its heat is not solar; it has more rocky components.
  • Neptune, despite being further from the Sun, generates more heat than it receives from the Sun. This heat is not solar and Neptune has the most rocky components among these planets.
85
Q

Origins of gas Giants: Core Accretion Model

A
  • This model involves the accretion of rock-ice planetesimals to form a core that is 10 to 20 Earth masses, which takes about 1 million years (Ma).
  • The next step is the accretion of a massive gaseous envelope, which takes between 1 to 10 Ma.
  • The problem with this model is that the nebula was all gone by 10 Ma after the start of the solar system.
86
Q

Origins of gas Giants: Disk Instability Model: (MORE LIKELY ONE)

A
  • This model involves the clumping of gas and dust in the disk.
  • There is a sudden gravitational collapse to form the planet, which takes only a few hundred or thousand years (within the first 1 Ma).
  • This model solves the problem of the nebula disappearing too quickly and is considered the most likely model for the formation of gas giants like Jupiter and Saturn
87
Q

What are the four moons of Jupiter?

A

– Io
– Europa
– Ganymede
– Callisto

88
Q

Io Volcanic features

A
  • Io is the most volcanically active body in the solar system
  • Volcanic pit craters, calderas, shield volcanoes and so on
  • there are umbrella shaped eruption Plumes
89
Q

Tidal heating in Io

A
  • Caused by gravitational interaction btw Jupiter and Io
  • Volcanic Activities: The heat generated from this frictional movement drives strong volcanic activities on Io’s surface
90
Q

Europa compared to Io

A
  • Io is closer to Jupiter, larger and denser
    ↳ Composed of silicates and sulfur
  • Europa is smaller, less dense and composed of silicates and water ice
  • Io has a slightly higher temp (118k vs 103k)
91
Q

Europa features

A
  • surface is characterized by fractured water ice with few craters
92
Q

Europa compared to ganymede

A
  • Ganymede is further from Jupiter & larger
  • Composition is the same but it has a higher temperature
93
Q

Ganymede Features

A
  • The surface of Ganymede is characterized by a
    dark, cratered terrain and a light, grooved terrain
    ↳ Dark cratered terrain is darkened by silicate
    ↳ Light grooved terrain is shallow but long
94
Q

Ganymede compared to Callisto

A
  • Callisto is a lot further away from jupiter
  • It is smaller with a similar denisty and same composition
  • Temp is very similar
95
Q

Callisto Features

A
  • The surface of Callisto is dominated by impact structures
  • Impacts onto an icy surface
96
Q

What causes the differences in the Galilean Satellites

A
  • The differences come with distance from jupiter
    ↳ Increase in surface ages
    ↳ Decreases in density

EAS 206 (7 decks)

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