Final: Ch 7, 15, 17, and 18 Flashcards
1
Q
how long ago did most of the objects in our solar system form?
A
4.5 BYA
2
Q
how much of the mass in the solar system is contained in the sun?
A
99.8%
3
Q
order of the planets from the sun
A
Mercury, Venus, Earth, Mars, Jupiter, Saturn, Uranus, and Neptune
4
Q
mnemonic for the order of the planets
A
My Very Educated Mother Just Served Us Nachos
5
Q
what is the most massive planet
A
Jupiter
6
Q
what direction do all the planets orbit the Sun
A
counter-clockwise from above the Sun’s N pole
7
Q
trans-Neptunian objects
A
objects farther out in the solar system
8
Q
dwarf planets
A
the largest trans-Neptunian objects including PLuto and the largest asteroids
9
Q
qualities of a planet
A
(a) is in orbit around the Sun
(b) has sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape
(c) has cleared the neighborhood around its orbit.
10
Q
qualities of a dwarf planet
A
(a) is in orbit around the Sun
(b) has sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape
(c) has not cleared the neighborhood around its orbit
(d) is not a satellite.
11
Q
what are the only planets without a moon
A
Mercury and Venues
12
Q
name the planet that the moon orbits:
- the moon
- the Galilean moons: Lo, Europa, Ganymede, and Callisto
- Titan
- Triton
A
- Earth
- Jupiter
- Saturn
- Neptune
13
Q
asteroids
A
rocky bodies that orbit the Sun, mainly in the asteroid belt between the orbits of Mars and Jupiter
14
Q
the Trojan (and Greek) asteroids
A
asteroids that share their orbit with Jupiter (because Jupiter’s gravity keeps them there)
15
Q
comets
A
small, icy bodies made of frozen gases that spend most of their time far from the Sun
16
Q
cosmic dust
A
countless pieces of “dust” (usually broken rocks) littered across the solar system
17
Q
meteor
A
when cosmic dust enters the atmosphere, it burns up, causing a brief flash
18
Q
meteorites
A
larger pieces of meteors that make it to the surface without burning up completely
19
Q
what are the planets named after
A
Roman deities
20
Q
what are the planet’s moons named after
A
Greek and Roman mythological figures somehow connected to the planet-deity (except Uranus, whose moons are named after characters in English literature)
21
Q
what are comets and asteroids named after
A
comets are usually named after their discoverers, while asteroids are named by their discoverers after whatever they like
22
Q
the giant planets
A
- Jupiter, Saturn, Uranus, and Neptune
- Uranus and Neptune are much small than Jupiter and Satun
23
Q
composition of Jupiter and Saturn
A
- mostly H and He
- Very small solid core of rock, metal, and ice
- Much of the H and He is compressed until it becomes liquid, so the next layer is “spherical ocean”
- Gaseous atmosphere that we see
24
Q
terrestrial planets
A
- Mercury, Venus, Earth, Mars
- All 4 are much smaller than the outer planets
- Composed of rock and metal
- Most of the heavier metals are in the cores
- The layered structure of terrestrial planets indicates that they were molten at some point
25
what is the most common rock in the terrestrial planets
Silicates (compounds of silicon)
26
what is the most common metal in the terrestrial planets
Iron
27
differentiation
The process in which materials are separated into layers according to density by gravity
28
what is the composition of moons?
- similar to that of their planets
- most are differentiated
29
are asteroids and comets differentiated?
no
30
Greenhouse effect
- Visible light easily passes through an atmosphere then planets absorb the light, heat up, and emit IR; the atmosphere blocks IR, keeping it in
- water and COs are molecules that absorb/block IR
31
what happened to Venus's atmosphere
had a “runaway” greenhouse effect
32
why are there no impact craters on Earth?
- internal forces that can change surfaces as well:
- Plate tectonics and volcanism
- Collectively, this is called geological activity
33
geological activity
- Driven by heat in the interior of a planet: heat escaping (or at least trying to) is what causes tectonic plate movement, volcanic eruptions, etc
- most terrestrial bodies were molten at one time, and a molten interior is what leads to geological activity
34
what is the correlation between impact craters and age of a planet?
- The more craters there are, the older the surface is
- The bigger the crater is, the more likely it is to be older
- If there is no geological activity, the age of the surface is the age of the planet
- If there is geological activity, the age of the planet will be older than the surface
- We can count craters on different parts of a planet’s surface to get the relative ages of those parts
35
radioactive decay
Some atoms are not stable, so over time, they decay into other, more stable atoms, giving off particles or gamma rays
36
half life
the time it takes for half the atoms in a sample to decay
37
how does the hald life dating process work
- Once we determine the half-life of a substance and its decay products (what it decays into) we can find the age of any sample
- From the original amount of the original substance to the decay product, we can find how many half-lives have passed, and then age
38
what is the relationship between a sun's rotation and its planets' orbits?
All planets orbit the sun in the same direction, which is also the direction of the sun’s rotation
39
solar nebula
rotating cloud of dust that the sun and all the planets formed from
40
building of a solar system
- solar nebula became a rotating disk, which then became the sun, planets, etc.
- Terrestrial planets and asteroids are all in the inner solar system (hot enough for gases and liquids to evaporate, but rocks and metals could survive)
- Giant planets, their moons, and comets are further out and have much more gas (cooler)
41
building a giant planet
clumps of gas move together randomly, their increased gravity pulls in more clumps, until you have a giant planet
42
building terrestrial planets
- rocks and metals form small clumps called planetesimals
- planetesimals combine to form planets via collisions that make them stick together
- eventually, an incredible multitude of planetesimals have combined, heated by their collisions and radioactive decay
- as the collection of planetesimals settles, differentiation occurs, and eventually the surface cools and solidifies into the crust of a terrestrial planet
43
planetesimals
rocks and metals from small clumps
44
what can explain the abnormal rotations of Venus, Uranus, and Pluto
the “abnormal” rotations of Venus (slow retrograde rotation), Uranus (on it side), and Pluto (on its side) can also be explained by these collisions: in the later stages of formation, a large (but not planet-sized) chunk of planetesimals might have hit the planet, reorienting its rotation axis
45
what is the size relationship between the sun and earth
it has a diameter equal to 109 times the diameter of the Earth, and thus a volume of about 1.3 million Earths
46
chemical makeup of the sun
73% hydrogen, 25% helium, 2% everything else
47
plasma
- hot ionized gas
- positively charged nuclei and negatively charged electrons
48
sun's core
- incredibly dense due to gravity
- it takes up about 20% of the Sun’s interior, has a temperature of about 15 million K, and it is where all the Sun’s energy is generated
49
source of the sun's energy
- nuclear fusion
- mainly occurs in the form of the proton-proton chain, a series of reactions involving collisions of hydrogen nuclei
- four hydrogen nuclei become one helium nucleus, giving off gamma rays and neutrinos
- the reason so much energy is released is that one helium nucleus has ever so slightly less mass than four hydrogen nuclei; about 0.71% less mass
50
layers of the sun
- core
- radiative zone
- convection zone
- solar photosphere
- chromosphere
- transition region
- corona
51
radiative zone
- extends out to about 70% of the Sun’s radius
- the light from the core radiates outward but makes very slow progress: before moving too far, it gets deflected by a particle, so it follows a “random walk” outward and loses energy in the process
52
convection zone
- extends to the surface of the Sun; it is about 200,000 km thick
- energy is transported outward by convection, not radiation
53
explain convection in the sun
the bottom of this zone is heated by the radiation, causing the plasma to rise upward toward the surface, where it loses energy to space, causing it to cool and sink back down, forming large loops of moving material, called convection cells
54
solar photosphere
- photons working their way out from the inner layers can finally move unimpeded by dense material
- ~ 400 km thick and average temperature of 5800 K
- much less density and pressure than Earth's atmosphere
- not uniform in appearance: it is composed of granules, bright regions with diameters of about 700-1000 km, divided from each other by narrow darker regions
55
"radius of the sun"
because the photosphere is where the Sun becomes opaque, the photosphere is the visible “surface” of the Sun, so when we talk about the “radius of the Sun,” we are talking about the distance between the center and the photosphere
56
granules
- bright regions with diameters of about 700-1000 km, divided from each other by narrow dark regions
- only last 5 to 10 minutes (photosphere changes rapidly)
- the tops of the convection cells below, and the dark areas, about 100 K cooler, are where the material sinks back down
57
chromosphere
- above the photosphere
- temperature around 10,000 K, hotter than the photosphere
- its spectrum of bright emission lines indicates it is composed of hot gases; because hydrogen dominates, the strongest emission line is H-α, which is red
- the spectrum of the chromosphere that led to the discovery of helium
58
transition region
- above the chromosphere
- the temperature rises from 10,000 K to over one million K
further, this region is less than 100 km thick
- we still do not know exactly how this temperature increase occurs
59
corona
- the outermost layer of the Sun’s atmosphere
- this layer is what is most visible during a total solar eclipse because it extends for millions of kilometers above the photosphere
- the photosphere is just so much brighter, which is why we do not see the corona all the time
- can also be viewed using a coronagraph on a space telescope: a circular disk is placed in front of the telescope to exactly cover the photosphere, just like the Moon does during a total solar eclipse
- the corona has a very low density (10^9 atoms per cm^3 at the bottom vs 10^16 atoms per cm^3 in photosphere and 10^19 molecules per cm^3 in Earth’s atmosphere at sea level)
- it also thins out as you get farther from the center of the Sun, but technically extends out extremely far, becoming the solar wind
60
solar wind
- a stream of charged particles given off by the sun’s atmosphere
- move outward at about 400 km/s
- the particles come from the corona: the particles are moving so quickly (due to the intense temperatures) that the gravity of the Sun cannot keep them bound
61
coronal holes
- the dimmer regions of the complex corona
- Most of the solar wind escapes from coronal holes
62
sunspots
- Dark regions on the surface of the sun, caused by magnetic interactions
- They appear dark because they are at a lower temp (3800K) than surroundings
- Larger sunspots have darker umbras surrounded by a lighter penumbra
- They usually appear in clusters of 2-20, or up to ~100
63
sunspots
- Dark regions on the surface of the sun, caused by magnetic interactions
- They appear dark because they are at a lower temp (3800K) than the surroundings
- Larger sunspots have darker umbras surrounded by a lighter penumbra
- They usually appear in clusters of 2-20, or up to ~100
64
what kind of rotation does the sun undergo?
- differential rotation
- Rotates at different rates at different latitudes
65
sunspot cycle
- During sunspot maximum, there can be 100+ sunspots visible at once
- During sunspot minimum, there might not be any
- full cycle lasts around 22 years
- polarities of leading spots flip each cycle
- That means that the overall magnetic field of the sun flips each cycle
66
Zeeman effect
When a magnetic field is present, each energy level of an atom gets split into multiple, very close levels, so spectral lines get split, too
67
sunspot effect on the magnetic field
the magnetic field is stronger at locations of sunsoits
68
why do sunspots appear in pairs?
- because magnetic N and S poles occur in pairs, each spot "represents" a pole
- Large groups of sunspots are complex, but the 2 principal spots play these roles
69
magnetogram
an image showing the magnetic field strength at each location
70
what creates the sun's magnetic field?
- The churning of solar material in the convective zone
- convection and differential rotation cause the field to get twisted up
71
where do sunspots form?
strong fields can form loops in field lines
72
why are sunspots cooler
because the strong field suppresses convection
73
plages
- bright "clouds" around sunspots in the chromosphere
- higher density and temp than surrounding material
74
prominences
- filaments of hot plasma near sunspots
- extend from the surface and into the corona
75
solar flare
- an eruption on the surface that releases a lot of material and energy over a short time
- near the maximum of the cycle, there can be several each day
- When fields of opposite polarity interact on the surface, they destroy each other, releasing the energy stored in the field
- Can trigger coronal mass ejections
76
coronal mass ejections (CMEs)
which material in the corona is flung away from the sun
77
active regions
areas near sunspots, caused by magnetic fields where solar flares and CMEs occur
78
space weather
solar wind, solar flares, and CMEs
79
what does solar wind do to Earth?
distorts earth’s magnetic field, which can cause minor EM disturbances on earth
80
what do solar flares do to Earth?
X-rays and charged particles can damage satellites
81
what do CMEs do to Earth?
- Bubble of matter and energy from CME heats the ionosphere, which expands putting more atmospheric drag on more satellites
- Even if satellites are physically effected, their signals can get distorted by CMEs
- A CME rapidly changes shape of Earth’s magnetic field, and changing magnetic fields produce electric fields and electric currents
- This can cause power surges, which can blow transformers, leading to blackouts
82
luminosity
- Total energy output across the entire EM spectrum
- Most fundamental measurement of a star’s brightness
- We often represent luminosity in terms of Sun’s
Lo = Lsun = 3.8 x 10^26 W
- Unfortunately, L cannot be measured directly
83
apparent brightness
- Only a small fraction of a star's energy reaches the earth
"the energy we receive from a star that hits x given area each second"
- Different brightnesses can be due to different factors:
- Different intrinsic luminosities
- Different distance
84
photometry
the process of finding brightness
85
Hipparchus's magnitude scale
- divided all visible stars into 6 categories or magnitudes
- Brightest: 1
- Dimmiest: 6
- The standard system made this exact: a difference of 5 magnitudes corresponds to a factor of 100 in brightness
- magnitudes go backward: higher magnitude means lower brightness
- Stars can have fractional magnitudes or negative magnitudes
86
brightness and mass equation
b2/b1 = 100^(m1-m2)/5
or
m1-m2 = 2.5 x log↓10(b2/b1)
87
star temp range
~2,000K to 40,000+K
88
Our Sun's temp
(5800K) peaks in greenish-yellow
89
A popular set of filters for color indices
U: (UV) 360nm
B: (blue) 420nm
V: (visible/yellow) 540nm
90
color indices
differences between colors
91
what are color indices at when a star is 10,000K
0
92
what causes different spectral lines being more or less prominent
different temps
93
what is the ideal star temp
~10,000K
94
spectral classes (spectral types) from highest temp to lowest:
- O, B, A, F, G, K, M, | L, T, Y
- Each class has 10 subclasses labeled 0-9 (0 being the hottest)
95
what spectral class is our sun in ?
G2
96
metals
all elements besides H and He
97
brown dwarfs
- Objects with temps below those of M9 are not “true” stars
- They have < 7.5% mass of the Sun, so they never get hot enough to have fusion occur like in the Sun
- about the same size as Jupiter, but range from ~13MJ to 80MJ
- Difference is brown dwarfs support deuterium fusions; planets do not
98
giants and supergiants
- very large stars
99
what is the relationship between star size and spectral lines?
- Larger star has narrower spectral lines than a smaller one
100
why does a larger star have narrower lines
- Larger star has larger photosphere, so the material has a lower density and pressure than that of a smaller star
- Lower density and pressure→ fewer collisions→ narrower lines
101
what is the relationship between star size and ionized material
- Larger star has more spectral lines from ionized material than small star at the same temp:
- # of atoms that get ionized depends on temp, so it is the same in both stars
- Atoms stay ionized longer in large star because low density makes it less likely that ion will interact with electron
- We will get stronger spectral lines from ions because the ions are around longer
102
metallioity
the fraction of a star that is composed of metals
103
proper motion
- motion of star across the sky relative to background stars
- These motions are incredibly small
- Measured in arc seconds per year
- If we also know the distance to the star, we can get its speed across the sky (transverse velocity)
104
how can we find radial velocity
doppler shift in spectrum
105
how can we find a star's space velocity
radial velocity and transverse velocity
106
rotation and Doppler shifts
- As long as an object’s rotation axis doesn’t point directly toward us, one side will move toward us and the other will move away due to rotation
- In star’s spectrum, rotation appears as line broadening: the faster the rotation, the broader the lines become
- It is due to different points on a star having different Doppler shifts
107
lightyear =
- 1 ly = 9.46 x 1012 km = 63,241 AU
- It is a unit of distance not time
108
why do most of the stars visible to the naked eye appear bright?
because they are many times brighter than our sun, but far awat
109
binary stars
- A system with two stars orbiti ng their common center of mass
- incredibly common
110
double star
- 2 stars that appear close in the sky
- It might be binary, but more likely, it is just a coincidence based on POV
111
visible binary
one that can be seen with a telescope
112
spectroscopic binary
- binary that is revealed by its spectrum:
- We get spectral lines of both stars together
- When one star is moving away (redshifted) and the other is moving toward us (blueshifted), we see both sets of lines
- When they are moving across our view, the lines lie on top of each other
- Consistent pattern of 2 sets of lines becoming 1 set and back indicates a binary star
113
how does Kepler's 3rd law relate to binary stars
- A^3 = (M1+M2) x P^2
- Spectrum gives us radial velocities, which gives us period of orbit
- With velocities and periods, we can find the distance the stars travel in one orbit (circumference of orbit) and thus semimajor axis
- This allows us to get total mass of both stars together
- Also with additional knowledge of the nature of the system, we can find the ratio of masses, and thus the individual masses
114
Mass and luminosity
- With some exceptions, luminosity scales with mass
- Mass-luminosity relation: states that L ~ M^3.9
- L/Lo = (M/Mo)4
115
stars blocked by the moon and size
- When the moon is blocking a star, the star dims, once the moon is fully blocking it, it disappears
- From the time that this process takes and known speed of the moon across the sky, we can find the angular diameter of the star
- If we know the distance to the star, we can find physical diameter
116
Eclipsing binary stars
- Relative depths in the dips incurve tell us about relative brightness
- Bigger dip, bigger eclipsed star
- When smaller stars start to pass behind (1st contact), curve starts to dip
- When “ “ disappears (2nd contact), we’ve reached the bottom
- When “ “ begins reappearing (3rd contact), curve starts to rise
- When “ “ has completely emerged (last contact), curve is back to a normal level
- Between 1st and 2nd contact, small star moves distance equal to its own diameter
- Between 1st and 3rd contact small star moves distance of big star’s diameter
- With those times and relative speeds of stars (from spectrum), we can find these distance
117
energy flux and luminosity relationship
- If 2 stars have the same temp (T1=T2), then F1 = F2
- Thus, any differences in L are due to differences in size
118
Luminosity and size relationship
-If we know luminosities (brightnesses and distances), then we can find sizes
- L1/L2 = R1^2/R2^2
119
The Hertzsprung-Russell diagram (D-R diagram)
- plots L vs T
- By convention, T increases to the left so that spectral types are in order
- Main Sequence: About 90% of all stars lie along a band from the upper left (High L, High T) to the lower right (low L, low T)
- Upper right is home to red/supergiants
- White dwarfs are located in the lower left of
120
proportions of Hertzsprung-Russell diagram
MS: ~90%
WD: ~10%
Giants: ~1%
121
proportion of a star's life that it spends at different stages
each star spends ~90% of its life on MS, ~10% of its life on WD, and ~1% on giants
122
what does main sequence correspond to
stars that are actively fusing H to He
123
mass relationship on the Hertzsprung-Russell diagram
High M→ high L, high T
Low M→ low L, low T
124
what happens when a star runs out of H in its core
- it contracts and expands as it fuses heavier and heavier elements, eventually becoming a red giant or red supergiant
- After all possible fusion reactions run out, gravity takes over completely, compressing a star into a white dwarf
125
white dwarfs
- High temps because they are so compressed
- not very luminous
- Masses comparable to Sun’s, but are around the size of earth, so they are extremely dense
- This is the last stage/end result for many MS stars
