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Post midterm ! Flashcards

1
Q

Protoplanetary disk inside frostline porpotions of materials..

A

0.2 metal
0.4 rock
1.4 hydrogen compounds
98 helium

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2
Q

Outside frost line porpotion of materials

A

0.2 metal (solid)
0.4 Rock (solid)
1.4 Hydrogen compounds
98 helium

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3
Q

Tiny small objects stick together to form

A

planetesimals

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4
Q

Planetesimals are the _____ of what will become planets

A

seeds

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5
Q

How does a crater form

A

planetesimal hits surface and vaporizes rock, creating explosion

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6
Q

heavy bombardment period

A

lots of planetisemals crashing everywhere after planets formed about 4 bil years ago

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7
Q

mercury and moon covered in

A

craters

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8
Q

LOOK UNDER SURFACE OF PLANET USING

A

SOUND WAVES

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9
Q

2 types of waves (vibrational travel)

A

P waves - compression

S waves - side to side

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10
Q

S wave paths

A

cant go past the liquid in the ball

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11
Q

what is the empty s wave parrt that cant be reached called

A

s - wave shadow zone

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12
Q

P wave paths

A

it goes through the liquid ball but everytime it goes through the curve of the line is like reflected

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13
Q

Timing for seismometers at different places depend on

A

how far and fast the wave traveled

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14
Q

Direction of ——– tell difference between S and P waves

A

vibrations

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15
Q

S wave on graph is

A

horizontal (east to west/ north to south)

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16
Q

P wave measured on graph is

A

verticle

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17
Q

Mercury is estimated from

A

density + spin rate variations

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18
Q

Venus is estimated from

A

density

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19
Q

Earth moon mars measured with

A

seismometers

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20
Q

Why do planets have cores

A

differentiation: lighter materials like rock float to top, heavier materails like iron sink

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21
Q

Why planet interiors hot:
accretion:

A

Dominant during formation

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22
Q

Why planet interiors hot:
differentiation:

A

more dominant earlier

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23
Q

Why planet interiors hot:
radioactive decay:

A

Dominant source of heat today

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24
Q

Planets cool via

A

convection

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25
Q

HOW PLANETS COOL step 1

A

convection:

Hot rock will rise, cool rock sink, hot rot goes surface and release heat

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26
Q

HOW PLANETS COOL step 2

A

Conduction:
carries the hot rock heat out cuz its thin and rigid

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27
Q

HOW PLANETS COOL step 3

A

radiation

energy gets radiated to space at surface as infrared light

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28
Q

smaller planets have less —— compared to surface area of a large planet

A

mass

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29
Q

craters get covered by, what does it indicate

A

molten lava spewing out and hardening, young surface

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30
Q

are any of earths craters result from heavy bombardement

A

no

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31
Q

mars has 384343 craters larger than _____km

A

1

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32
Q

Mares on the moon are

A

dark spots that used to be craters but got hard lava covered it

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33
Q

Mars has many volcanoes that are

A

NOT ACTIVE

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34
Q

Small terrestrial planets interior cools… leading to……

A

rapidly

quickly ending volcanic activity

lack of volcanic activity means no outgassing cuz low gravity allows gas to escape –> no atmosphere

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35
Q

LAck of volcanic activity on small terrestrial planets means

A

low outgassing, so gas leaves really easily and does not form atmosphere leading to NO EROSION

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36
Q

large terrestrial size and stuff is

A

opposite of little planet:

Slow cooling

volcanic activity

has atmosphere?

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37
Q

outgassing produces

A

atmosphere

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38
Q

Temperature changes can put stress on planets crust causing. (2things)

A

mountains and cracksq

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39
Q

PLate tectonic workings:

Subduction at CONVERGING plates

A

ocean plates get pushed under continent plates, making the continental plates high (mountain)

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40
Q

PLate tectonic workings:
diverging plates

A

causes undersea ridges

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41
Q

No erosion likely means

A

water stopped flowing

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42
Q

Trend in terrestrial planet atmospheres

A

larger planets have thicker atmospheres

NO h2 in the atmosphere

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43
Q

Higher temperature means what for average speed

A

faster average speed

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44
Q

higher mass means what for avg speed

A

slower avg speed

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45
Q

Objects going faster than a planets escape velocity will…..

A

escape into space

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46
Q

lower mass planets have lower…. soo….

A

escape velocity, easier to escape

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47
Q

It is easier to escape a —– planet’s gravity

A

small

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48
Q

low mass gas moves….. so…

A

faster, easier to escape

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49
Q

Hot gas moves…… so…..

A

faster, easier to escape

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50
Q

Mercury + Moon escapes velocities are

A

low

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51
Q

Venus escape velocity is

A

high

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52
Q

Mars escape velocity is

A

in the middle (between mercury and venus)

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53
Q

venus, mars, merury, moon escape velocities are all

A

too low to keep H2

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54
Q

Carbon cycle on earth (why is N2 left as dominant gas)

A

Co2 in air dissolves in rainwater

water flows into ocean with minerals

Co2 in water reacts with rocks/metals to form CARBONATE ROCKS

carbonate rock is pushed to ocean floor under tectonic plates

volcanos releases small amounts of this co2 back into atmosphere

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55
Q

why doesn’t earth have much CO2

A

it has water

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56
Q

Co2 levels on earth vary based on

A

volcanism

biological activity

have ben dropping for the past 50 mil years

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57
Q

The warmer the planet, the more ———– —— is emitted

A

infrared light

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58
Q

The planet will warm until the absorption of ——— —– and emission of —— —— are balanced

A

visible light

infrared light

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59
Q

Visible light from the sun shines on planet, some light is ——— and the rest is ——–

A

reflected (as infrared)

absorbed

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60
Q

Greenhouse effect (think of how blanket works)

“No u”

A

visible light gets in the atmosphere which is mostly absorbed and the planet gets hot so infrared light is emitted and the greenhouse gasses absorb and remit this back onto surface (blanket)

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61
Q

venus is EXTREMELY hot because

A

thickass atmosphere, traps lots of heat, greenhouse gas effect

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62
Q

PHOTODISSOCIATION:

– light from sun separates atmospheres’ ——

A

UV

atoms

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63
Q

PHOTODISSOCIATION:

the separated atoms from the UV light will——– asap after ——— each other

A

reconnect

refinding

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64
Q

individual atoms are lighter than molecule so……

A

can escape easier

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64
Q

Solar wind of high energy particles do what to the atoms on mars

A

knock thema way

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65
Q

define crust

A

low density rock

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66
Q

core

A

high density iron/nickel

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67
Q

mantle

A

medium density rock

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68
Q

Earth’s magnetic field deflect solar wind particles which…

A

stops the atmosphere from breaking

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69
Q

Asteroids orbit……….. they are not large enough to be…..

A

the sun

spherical

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70
Q

half an elliptical is called (YELLOW LINE DIVIDING ELLIPSE)

A

SEMI-MAJOR AXIS

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71
Q

Time of an orbit (period) depends on

A

semi major axis

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72
Q

Jupiter effects the —— of the asteroids

A

orbits

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73
Q

Orbits in —— ———— with Jupiter get ———

A

exact resonance

displaced

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74
Q

The displaced asteroids form —— — along the ring meaning that there are — asteroids

A

dark bands

no

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75
Q

Largest object in asteroid belt

A

Ceres

76
Q

Ceres inside has

A

liquid brine, icy crust, rocky center

77
Q

Vesta is —— asteroid

A

largest

78
Q

kuiper belt is x times —– than asteroid belt

what does it include

A

20-200 times more massive than asteroid belt

includes several dwarf planets

79
Q

where was kuiper belt formed

A

outside of frost line

80
Q

Oort cloud

A

huge spherical cloud of comets

81
Q

Comets in oort cloud were formed near ——– but kicked out by ———- ———

A

JUPITER

gravitational interactions

82
Q

how many objects in oort cloud

A

trillions

83
Q

meteorites are

A

asteroids that hit earth

84
Q

Outside frost line, — temperature allow ——— planets to include —— molecules like H20m Nh4 and Ch4

A

low

condensing

volatile

85
Q

Where are Terrestrial planets formed inside

A

INSIDE FROST LINEEE

86
Q

Juno space probe is doing what rn

A

orbiting jupiter

87
Q

Jupiter inside

Before impact:

Just after impact:

Present day:

A

Dense core

dilute core

Well developed dilute core

88
Q

Hydrogen can turn form gas to liquid to metal if……… who has this?

A

theres enough pressure

Jupiter has towards the center

89
Q

Ammonia clouds are what colur

A

white

90
Q

What varies as you enter jupiter?

A

temperature and pressure

91
Q

Red bands on jupiter are lower——— clouds, which are ———- and brighter

A

altitude

warmer

92
Q

White bands on jupiter are higher—- clouds which are ——- therefore emit —— infrared light

A

altitude

cooler

less

93
Q

Saturns hexagon has a huge what

A

hurricane

94
Q

Saturns rings are over ——km but less than —km thick

A

260,000

0.1

95
Q

Neptune and uranus are called ice giants because

A

they are big with icy and rocky cores

96
Q

Neptune is

A

furthest from sun

28 degree tilt

strongest winds

97
Q

Uranus

A

coldest planet

thick water + ammondia + methane mantle

98
Q

who has thick water + ammondia + methane mantle

A

uranus

99
Q

very old created surface mostly made of ices, thin brown layer over ice with giant ridge

A

Iaeptus

100
Q

one of most reflective object in solar system (HIGH ALBEDO)

A

enceladus (a saturn moon)

101
Q

what does high albedo mean

A

highly reflective surface

102
Q

Heavily cratered, very porus (40% empty space), made of ice water

A

HYPERION

103
Q

When farther from jupiter, tidal forces are

A

less

104
Q

When closer to jupiter, tidal forces are

A

more

105
Q

The relationship between the tidal forces when close and far away from jupiter causes ——. This is also called —— ——-. This removes ——— out of orbit so it gradually becomes circular

A

friction

tidal heating

energy

106
Q

Gravitational tugs by Europa and Ganymede (fellow moons) does what to its fellow moon

A

Makes IO’s orbit still elliptical

107
Q

Small moon —— creates the —– gap via what resonance ratio

A

mimas

huygens

2:1

108
Q

bascially moons cause what on rings

A

deflect particles out of that ring within saturns ring

109
Q

Waves on the disk (saturns ring) also caused by

A

tiny moon making thin gap

110
Q

Not all wavelengths of light are allowed to travel….

A

travel through the atmosphere

111
Q

On atmospheric absorption graph, 0 means

A

no light reaches surface

112
Q

turbulence in earths atmospheres distorts the….

A

images we see from telescopes

113
Q

For long exposure and large telescopes, turbulence…

A

blurs image

114
Q

HOBBLE telescope

A

telescope in earths orbit that is above the atmosphere, 5-10x better resolution

115
Q

How did voyager probes use planets gravity to advantage (think slingshot)

A

When they lined up, it used each planets gravity to accelerate or slingshot itself to the next

116
Q

Transfer orbit steps

A
  1. start in inner orbit
  2. engine burn to speed up
  3. Now in the transfer orbit
  4. Do a 2nd burn to speed up
  5. end in outer orbit
117
Q

when is fuel used during transfer orbit. whats happening when ur not using fuel?

A

fuel used when you boost in step 2 and 4.

Laying in orbit

118
Q

Inner solar system uses solar pannels to convert ——-to ——-

A

sunlight]\

electricity

119
Q

Outer solar system uses RADIOISOTOPE THERMOELECTRIC GENERATOR TO generate electricity using

A

radioactive plutonium

120
Q

Exoplanet means

A

a planet orbiting star thats not sun

121
Q

star NAME then “NAME a”, “NAME b”, “NAME c”

A

Naming system for exoplanets

122
Q

exoplanets are very faint compared to their

A

parent star

123
Q

through a standard microscope, exoplanets are

A

essentially invis

124
Q

Exoplanets are hard to see directly beacause

A

the parent star bright light shining coveres them

125
Q

Indirect methods

A

transit method (2969 planets found)

doppler method/radial velocity (863 found)

126
Q

when one celestial object passes in front of another from our POV it is called

A

a transit

127
Q

seeing Venus in front of sun from earth (OUR POV) is example of

A

transit

128
Q

Transit method measures the

A

light curves

129
Q

transits only occur if the planets orbit happens to be

A

edge on as viewed from earth

130
Q

A dip on the transit graph tells us

A

a planet blocking the brightness of the parent star (EXOPLANET!!!)

131
Q

the deep dips are ——— and the half way deep dips are ——–

A

planet transits

eclipses

132
Q

THE DEEPER THE TRANSIT,….

A

THE BIGGER THE EXOPLANET

133
Q

Difference between night and day sides of transits give us

A

Temperature

134
Q

Getting exoplanets spectrum

A

(Star + planet spectrum) - (star spectrum) = Exoplanet spectrum

135
Q

What is KEPLER

A

a transit machine

136
Q

why is kepler useful

A

the transits it records is much cleaner

137
Q

Find periodic spacing by

A

seeing the big dip and finding the half of it, then finding smallest dip and finding the double of that

138
Q

For multiple planets periodic spacing has a requirement, whats that

A

planet 2 has to be bigger and block more light

139
Q

KEPLER HAS SHOWN THAT THERE ARE MANY MORE —– THAN —– EXOPLANETS

A

SMALL

large

140
Q

small exoplanet numbers are all HUGE underestimates because

A

smaller ones are harder to findddd

141
Q

large exoplanet numbers are also underestimates because

A

they have long orbital periods so maybe we aren’t observing for long enough to know

142
Q

weakness of transit

A

can only see exoplanets edge on

needs continuous monitor

biased towards close-in

only way to find small exoplanets is from space

143
Q

overal transit method gives us….. of exoplanets

A

Size

Temp

Periodic spacing

Spectrum

144
Q

Strengths or transit method

A

does not need big telescope

can detect very small exoplanets

ONLY way to measure size

atmospheric composition

145
Q

IF exoplanets have extra moons or rings, we would see

A

extra very small dips like super small in the original dip

146
Q

Doppler effect for light:

A

Spectra

147
Q

Redshifted lines

A

moving away (longer wavelength0

148
Q

Blueshifted lines

A

Moving closer to us (shorter wavelength)

149
Q

more severe blue/red shift towards either direction means

A

speed is faster

150
Q

Doppler only measures line of sight:

For object moving DIRECTLY away, we measure

A

all its speed

151
Q

Doppler only measures line of sight:

For object moving ACCROSS line of sight, we measure

A

none of its speed

152
Q

Doppler only measures line of sight:

objects moving diagonally

A

Only part of its speed

153
Q

The only part of motion we can measure in all cases of Doppler line of sight measures is called

A

radial velocity

154
Q

KEPLERS 1ST LAW OF ORBIT

A

Planets orbit sun in elliptical , with sun at focus

155
Q

why is keplers first law wrong

A

Planets and stars BOTh orbit the center of mass, but stars are so big that they don’t move much

156
Q

Why don’t stars move much when orbiting centre of mass

A

they are so massive that usually they are basically/veryclose to the centre of mass

157
Q

A star wobbling towards and away from us is

A

What our POV sees when a star is “orbiting” the centre of mass

158
Q

exoplanet moves in large orbits but cannot be seen

parent star moves in tiny orbits and is bright enough to see

how can doppler affect be applied

A

using doppler effect to the spectrum of the star to measure the radial velocity (WOBBLE) of the star as it orbits

159
Q

Doppler method observes the spectrum of the —– NOT the ——

A

star NOTT

planet

160
Q

Keplers third law

A

p^2/m^2 is same for all planets

161
Q

Most common type of exoplanet found in BOTH search types jupiters

A

HOT JUPITERS

162
Q

51 peg b

A

first exoplanet found, 0.53 AU

half the mass of jupiter, but closer to sun

163
Q

hot jupiters current thinking

A

they FORM in outer system, move inward

164
Q

term for “formed in outer system, move inward”

A

planetary migration

165
Q

Hot jupiters are common because

A

they are easier to find, they make deeper light scale deeps.

166
Q

Hot jupiters are heavy and close-in meaning for doppler,

A

they produce large wobble in parent star

167
Q

Hot jupiters are heavy and close-in meaning for TRANSIT,

A

they make deep transit in parent star’s light curves.

168
Q

term for “wobble or transit repeats quick”

A

Close-in

169
Q

Hot jupiters dominance is an

A

observational bias

170
Q

Is it usually possible to detect inclination of the orbit

A

nope

171
Q

we only have a lower limit on true doppler velocity,

we only know the minimum possible mass of exoplanet

WHEN……

A

when we find an exoplanet via doppler method

172
Q

If exoplanet als transits, we know it must be orbiting nearly ———-, so we know its actual —— and ——

A

EDGE ON

mass and size

173
Q

doppler weakness

A

neeed big telescope

only measure minumum mass unless we know inclination

only study one star at a time

173
Q

doppler method strenght

A

no continuous monitor

works for any orientation (besides face-on)

very good for massive planets in close-in orbits

174
Q

Combining transit method (size and inclination) and doppler method (mass) gives us

A

density

175
Q

dotted lines on graph plots mean

A

various possible densities

176
Q

solar system planets on graph plots are what colur

A

green

177
Q

selected transiting exoplanets are what colour

A

red

178
Q

kepler 11f

A

same mass as earth but twice the size

179
Q

kepler 10b size and density

A

double size of earth

similar density to lead

180
Q

Angular size of an objet depends on

A

how big and far away an object is

181
Q

LIFE IS EVERYWHERE IN UNIVERSE, GETS TRANSPORTED FROM NEW ASTWROUDS

A

PANSPERMIA

182
Q

LUFE AROSE ON EAERTH FROM NATURAL PROCESSES, INORGANIC MATERIAL CONVERSIONS

A

ABIOGENESIS

183
Q

nutrients (easy)

Energy - sunlight, heat etc (easy)

liquid water (HARD)

A

requirements for life

184
Q

Habitable zone

A

orbits where a terrestrial planet could have liquid water on surface

185
Q

What are ESI scores

A

earth similarity index 0-1, based on exoplanets similarity to earth

186
Q

FERMI PARADOX

A

optimisitc view of the drake equation

187
Q

drake equation

A

of intelligent civilizations =
Nhp x f life x fciv x fnow

ast (2 decks)

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