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AST101 > AST Pre-Midterm > Flashcards

AST Pre-Midterm Flashcards

1
Q

all planets orbit the same _______ ______

A

ecliptic plane

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2
Q

what direction does planet orbit

A

same direction with elliptical orbit

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3
Q

Sun rotation is

A

same direction as planet

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4
Q

Terrestrial planet charcteristics

A

Small & rocky

thin/no atmosphere

few moons

heavy elements

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5
Q

Jovian planet charcteristics

A

Large gas/liquid

many moons

Lighter elements

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6
Q

Mercury simple stats

A

no moons, highly cratered

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7
Q

Venus stats

A

Thick Co2 atmosphere

460C surface T (greenhouse effect)

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8
Q

venus rotation is what

A

ROTATE BACKWARDS

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9
Q

Earth stats

A

No2 atm

23.4 degree tilt

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10
Q

Mars stat

A

2 moon

thin co2 atmosphere

25.2 tilt

polar ice caps

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11
Q

Jupiter stat

A

Over 60 moons

thick gaseous atm

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12
Q

Saturn stats

A

Over 60 moons

similar structure to jupiter

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13
Q

Uranus

A

Thin rings
98 tilt
Coldest

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14
Q

Neptune stats

A

Wispy clouds

winds up to 2000km.hr

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15
Q

pluto ice content is

A

high

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16
Q

asteroid belt

A
  • millions of asteroids between mars + jupiter
  • 3% of earths moon
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17
Q

Kuiper belt

A

icy bodies around neptunes orbit

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18
Q

comets

A

small icy bodies with elliptical orbits

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19
Q

Mars thin Co2 causes

A

planet wide storms

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20
Q

Summer time

A

daylight longer, sun higher,

–> more direct

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21
Q

Winter time

A

days shorter, sun is lower

–> shallow angle

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22
Q

Summer/winter solstices based on

A

north being covered or lit up all the time

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23
Q

equinox are

A

when sun shine equally on both poles so 12 days

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24
Q

Solar eclipse

A

moon block sun

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25
Q

Lunar eclipse

A

earth block moon

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26
Q

moons orbit is tilted why

A

to avoid eclipses every month

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27
Q

Solar eclipse angle requirment

A

when earth orbit changed by 90 (when tilt of earth and moon align)

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28
Q

Only time solar eclipse can happen

A

New moon

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29
Q

New moon

A

invisible

rise and set with sun

only time solar eclipse can happen

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30
Q

Waxing cresent

A

3-4 days after new moon

rise +set 3 hours after sun

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31
Q

waxing cresent easiest to see

A

after sunset

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32
Q

Waxing quarter

A

1 week after new moon

rise + set 6 hours after sun

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33
Q

Waxing gibbous

A

10-11 days after newmoon

rise set 9 hours after sun

easiest at night. might set before sunrise

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34
Q

full moon

A

2 week after new moon

rise set 12 hours after sun

invisible most of night

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35
Q

Waning gibbous

A

10-11 days before NEXT nm

rise before midnight, up rest of night

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36
Q

Waning quarter

A

1 week before NEXT nm

6 hours set /rise before sun

rise around midnight

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37
Q

Waning crescent

A

2-4 days before next newmoon

rise around 3 hours before sunset

easiest to see before sunrise

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38
Q

Farther away in avocado elliptical diagram means

A

SLOWER, farther away, less distance to be covered

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39
Q

Closer in avocado elliptical diagram means

A

closer, more distance needs to be covered so FASTER

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40
Q

speed

A

rate of change

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41
Q

velocity

A

rate of change + direction

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42
Q

acceleration

A

rate of change of velocity

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43
Q

Kepler’s First Law

A

The orbit of each planet about the Sun is an ellipse with the Sun at one focus

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44
Q

Kepler’s Second Law

A

A planet moves faster near the sun and slower farther from the sun

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45
Q

Kepler’s Third Law

A

More distant planets orbit the Sun at slower average speeds

It obeys: T = 365.24 √r^3

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46
Q

newton 1st law

A

object in motion stays in motion

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47
Q

Newton 2nd law

A

F=ma

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48
Q

Newton third law

A

equal and opposite force reciprocation

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49
Q

angular momentum formula

A

L = = iW= mvr

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50
Q

whats angular momentum explain w example

A

arms out, spin slow, arms in, spin faster

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51
Q

in F = (G m1m2)/d^2

double mass =

A

double force

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52
Q

in F = (G m1m2)/d^2 double distance

A

4x LESS force since it would be over 2^2

53
Q

in F = (G m1m2)/d^2 , 1/2 distance

A

4x MORE force since its (1/2)^2 and your dividing by a fraction.

54
Q

explain tidal force moon and earth relationship

A

Tidal force ON MOON FROM EARTH is larger than the force of MOON ON EARTH

(earth puts more tidal force on moon than the moon puts on earth)

55
Q

tidal force:

A

The earth puts more force on the moon that it slows down rotation so much it became locked

The earth same side of moon always faces earth due to tidal forces

56
Q

TIDAL RELATIONSHIP is _______. This causes _______ and __________ rotation

A

laggy

delays

slower

57
Q

Spring tide (LARGE)

A

when the suns tidal forces line up with the moon and earths

58
Q

what phase of the moon is spring tide

A

Full or new moon

59
Q

how many high and low tides per day

A

2 each

60
Q

What phase of the moon is neap tide

A

First quarter + third/last quarter

61
Q

What is happening during a neap tide

A

In a quarter moon, sun and moon tidal forces cancel out partially

62
Q

what angles are SUN and MOON during neap tide

A

right angle

63
Q

Why does sun shine

A

nuclear fusion in core converting H into He & releasing energy

64
Q

Core of sun

A

15 mil degrees

where nuclear fusion occurs

contains 50% of suns mass, 25% suns radius

65
Q

where does nuclear fusion occur

A

core of sun

66
Q

Radiative zone

A
  • extends from 25% to 70% of suns radius

-49% of suns mass

  • light and heat travel out from core (4million degrees)
67
Q

Extends from 25% to 70% of suns radius

A

radiative zone

68
Q

light and heat travel ____ from core into ______ _____ (4million degrees)

A

out

radiative zone

69
Q

Connective zone

A
  • outermost, extends 70%-100% radius
  • ONLY 1% of suns mass
  • least hot
70
Q

Least hot zone in sun, why?

A

connective zone, lots hot gas rise then churn

71
Q

percentage mass of zones:

core

radiative zone

Connective zone

A

50% mass

49% mass

1% mass

72
Q

Photosphere (miso soup) =. visible ______ ______ from _______ to ________

A

surface changes

transparent

opaque

73
Q

how does photosphere surface change/look like

A
  • granulated
  • hot areas rise, cold areas sink
  • particles form gas flow out, filling solar wind
74
Q

what is the photosphere as a part of the sun

A

SURFACEEE!!!!

75
Q

Sunspots

A
  • comes in pairs (suns balls for cooling)
  • cooler regions
  • only 3500C
76
Q

photosphere temp

A

5500C

77
Q

core of sun temp

A

15mil Celcius

78
Q

radiative zone temp

A

4mil ish C

79
Q

Conective zone temp

A

2mil celcius

80
Q

why are sunspots cooler parts of sun

A

cuz magnetism prevent hot gas from rising (you need to diarhea but you clench it)

81
Q

Chromosphere (thin)

A

right above sun “surface”

reddish glow, low density

82
Q

Corona

A

halo of gas ABOVE chromosphere and photospere

83
Q

Corona only occurs only

A

during total eclipse

84
Q

The —— in the corona allows —– —- to escape

A

halo

solar wind

85
Q

Fusion

A

happens in light elements like helium

86
Q

fission

A

heavy elements

87
Q

Nuclear fusion is hard to make happen because

A

the protons repel

88
Q

P-P energy

A

chance of 4 protons colliding (energy)

89
Q

Positron

A

like an electron but with a + charge

90
Q

Neutron:

A

ow mass but neutral charge

91
Q

Gamma ray

A

type of light

92
Q

Hydrostatic equilibrium

A

The core of star is very hot so it puts pressure out, but the gravitational pull counteracts it and pulls the star inwards

93
Q

is hydrostatic equilibrium only in stars

A

no , planets have it too, thats why they round

94
Q

Whats light

A

Electromagnetic wave that oscillates on wavelength

light has wavelegnth and frequency

95
Q

wavelength measure

A

distance between 2 peaks

96
Q

Frequency measure

A

of times in 1 second a peak pass

97
Q

Interstellar medium

A

gas (mostly h and he) and dust between stars

98
Q

molecular clouds as part of interstellar medium

A

Most dense part of interstellar medium, where stars are born

99
Q

Molecular clouds

A
  • cold and dense, enable star formation by gravitational collapse
  • contain dust that blocks starlight (appeares black)
  • molecules are formed in the dust grains, some being building block of life
100
Q

gravitational collapse

A

inward pull of g really strong

101
Q

Star formation

A

begin with gravitational collapse of moleular cloud

protostar form out clouds center as gas collapses and heat up

102
Q

3 ways molecular clouds are unique

A
  1. hydrogen in molecular clouds are molecules yet an atom everywhere else
  2. Molecular clouds are big enough to affect themselves and surroundings
  3. Only known place in UNIVERSE where stars form
103
Q

how did sun form

A
  • Something start molecular cloud collapse
  • gravity drags it in
  • gravity overcomes outward pressure in gas cloud (only in cold and dense areas)
104
Q

high density area in cloud

A

strong pressure out

105
Q

low temperature

A

low pressure out

106
Q

In cloud fragments, ______ mass of one molecular cloud is enough for ________________ stars formation

A

total

thousands of

107
Q

Small clumps/fragments of clouds become more pronounced, then…..

A

clouds fragment into separate clouds that continue to collapse and form stars

108
Q

Molecular cloud process summarized

A
  1. Cold dense clouds get pulled in by gravity –> increases the density
  2. as the cloud collapses, gas compressions heat up cloud, molecules in gas collide to make photons
  3. some photons escape until becomes too dense, they (heat) get trapped and start slow down collapse
  4. at core, protostar forms ,increase mass as gas falls in
109
Q

jets

A

protostars have jets of material that blow away surrounding gas: nakedness

110
Q

Accretion disk

A

during collapse, gas rotationand looks like a flat disk egg

  • hotter and faster than protoplanetary disk
111
Q

Protoplanetary disk

A

new planet birth sites

112
Q

light is a

A

wave but also a particle

113
Q

our eyes see

A

absorption

114
Q

—— determines colour

A

wavelength

115
Q

list lights in order of least energy

A

radio < microwave < infrared < visible < uv < xray < gamma

116
Q

we emit light via

A

thermal radiation

117
Q

Blackbody radiation:

——- decides everything

hotter = (2 things)

A

Temp decides everything

brighter, bluer

118
Q

On a blackbody graph, colder is

A

lower/ smaller line

119
Q

on blackbody graph, hotter is

A

bigger graphs, with SHORTER WAVELENGTHS

120
Q

example of red light that not hot

A

red shirt SCATTERS red light, but its not 3000C

121
Q

If light is black, a graph will show

A

dip to 0

122
Q

light tells us

A

temp + composition (what you emit/absorb)

123
Q

Doppler effect of light:

If something moving towards you,

A

it looks bluer, as its shifted to a higher frequency

124
Q

Doppler effect of light:

when something moves away form you

A

Things look redder, as longer wavelength

125
Q

redshift in spectra =

A

moving away from something

126
Q

blueshift in spectra =

A

moving towards something

127
Q

Measures of line of sight:

Direct

Across line of sight

Diagonally

A

can be measured

non measured

partially measured

128
Q

solar flare

A

sudden burst of energy + radiation into space

AST101 (1 decks)

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