Chapter 10,11,12,13 Flashcards

1
Q

what does the nebular theory tell us about the giant planets?

A
  1. Giant planets must form quickly
  2. Giant planets must form beyond the frost line
  3. Gas giants should have solid cores of ice and dust. these should be 10 earth masses since this is the threshold for runaway recreation of gas.
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2
Q

Structure of gas planets

A

top-down: atmosphere crust mantle and core.
high pressure in the interior causes phase of hydrogen to change with depth. At highest pressure, selectrons can stream freely acting like metals

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3
Q

facts about Jupiter

A
  1. Jupiter’s core is not dense, solid mass at center
  2. solid materials mixed with gas out to 1/2 radius
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4
Q

How are mass and pressure linked

A

more mass compresses the gas making it smaller

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5
Q

What causes colours on Jupiter and Saturn

A

Ammonia is the highest coldest layer and it reflects all colours hence the white look
Ammonium sulphide clouds reflect red/brown colour and these form at lower altitudes where its hotter.

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6
Q

Wind pattern of gas giants

A

all four planets have differential rotation but Uranus and Neptune are simpler and more like Earth

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7
Q

Jupiter and storms?

A

Jupiter has some of the longest-lived storms

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8
Q

How are moons formed?

A

moon formation is the same as planet formation but smaller

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9
Q

IO and volcanic activity

A

Io has evidence of volcanic activity due to tidal heating these effects are weaker the further away you go

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10
Q

Europa’s geology?

A
  • Euphora has lots of water ice available during formation
  • Tidal heating acts on Europa too but to a lesser extent than Io
  • Extra heat allows for liquid water ocean below the surface of Europa.
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11
Q

What two moons have evidence of water?

A

Both Europa and Ganymede show measurement changes in the magnetic field suggesting both moons have liquid water oceans beneath icy crusts

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12
Q

Titan Saturn’s largest moon

A

titan is the only moon with an atmosphere and is the second-largest moon in the solar system. that said it is likely covered by Saturn’s magnetosphere since it doesn’t have its own magnetic field

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13
Q

Enceladus (medium moon of Saturn)

A

ongoing cryovolcanism - eject water vapours and ice particles. Evidence of liquid water below the icy crust

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14
Q

Moons breakdown

A

see image:

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15
Q

Rings around gas planets

A

Saturn’s rings are very thin and consist of ice and boulders, these particles collide and sometimes stick together. any particles with incline collide more often also losing their incline. Bright regions have higher particle density whilst darker regions have lower particle density.

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16
Q

Velocity and distance

A

The more distant planets orbit the sun more slowly. suggesting closer objects orbit faster and have higher velocities

17
Q

How do rings prevent moon formation

A

only very small moons can survive in tidal forces close to Saturn. Collision with ring particles knocks off dust and debris from the moon to resupply rings.

18
Q

What is Roche limit

A

see image:

19
Q

Asteroids and comets

A

An asteroid is made up of silicate rocks, iron and nickel some have carbon-rich material. Comets are made up of silicate rocks, iron and nickel and hydrogen compound ice.

20
Q

What are the requirements to be considered a planet?

A
  1. Must orbit the star, not another planet
  2. must be large enough to be spherical in shape
  3. must have cleared the orbit of debris.
    Dwarf planets do the first two but not the third
21
Q

effects of a huge impact

A
  1. dust and debris from the impact was spread over most of north America
  2. dust and ash filled the atmosphere, blocking sunlight and cooling the planet’s surface, killing plants at the base of the food chain
  3. nitrous oxide was produced that acidified the oceans
  4. heat from impact ignited volcanic eruptions which produced more ash.
22
Q

what happens when a comet approaches the sun

A

Icy material starts to vaporize, releasing gas and dust particles in a coma around the frozen nucleus. This develops two tails: the Plasma Tail of ionized gas particles pushed directly away from the sun by the solar wind. The dust tail of rocky particles pushed more gently by solar radiation.

23
Q

What are two ways to find exoplanets?

A
  • direct method: actually see light from the planets
  • indirect method: Detect the planets via their impacts on other objects.