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SC120 > Final > Flashcards

Final Flashcards

1
Q

Protoplanetary Debris Disk

A

observed infrared disk around some stars
object collision dust
cold, low-density, around later stage older stars on the Main Sequence
Many have details of structure and shape, likely formed planets

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2
Q

Infrared Spectra Brightness Change

A

a method for seeing the transit of a planet across a distant star
same technique used to detect eclipsing binary stars

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3
Q

Doppler shifts

A

used to measure the spectrum changes of star

same technique used to study spectroscopic binary stars

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4
Q

Transit

A

when star luminosity drops as a planet passes in front of a star, observer must look along ecliptic

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5
Q

Habitable zones

A

distance from a star where water and atmosphere are possible

NASA Kepler Mission discovered several possible planets in habitable zones

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6
Q

Extrasolar Planet (Exoplanet)

A

planet orbiting a star other than the Sun

Faint and difficult to detect

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7
Q

Interstellar medium (ISM)

A

low-density clouds of gas and dust between stars (similar to Sun composition)
75% hydrogen 25% helium, traces of C and heavier things

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8
Q

Interstellar dust

A

smoke sized carbon, silicates, H2O ice coat, organization compounds

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9
Q

Dense Cloud

A

Cooler clouds pushed by warmer air currents called hot low density gas

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10
Q

Emission Nebula

A

excited by B1 or hotter near star to produce spectrum, glow pink, also called HII regions
ionized nuclei and free electron mixed, nucleus captures electron that fall through energy levels

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11
Q

Reflection Nebula

A

starlight scatters from a dust nebula, reflected absorption spectrum of starlight, appear blue because short wavelength scatters more easily

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12
Q

Dark Nebula

A

dense cloud obscuring distant stars, breezes and currents twist and distort them
stars seen through cloud are redder because dust scatters blue light

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13
Q

Interstellar reddening

A

stars seen through dark nebula are redder because dust scatters blue light

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14
Q

Molecular Cloud

A

dense clouds where atoms are able to link together forming molecules

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15
Q

Bok globules

A

small dark cloud containing 10 to 1000 solar masses of gas, thought forming star

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16
Q

Shock wave

A

travelling sudden change of pressure, can disrupt/compress cloud, causing birth of a very hot star

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17
Q

Birth of a Star

A

shock wave agitates gas
birth of very hot star that emits UV photons
drives away cloud
can also trigger star formation

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18
Q

Star cluster

A

stable group of stars held together by combined gravity orbiting common center of mass

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19
Q

Stellar Association

A

groups of stars formed together but not gravitationally bound, so drift apart
youngest rich in O and B stars

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20
Q

Protostar

A

as gas gets added, a warm ball destined to become a star, buried deep in dusty cloud
contraction converts gravitational energy into thermal, half radiates into space

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21
Q

Herbig-Haro object

A

small flickering nebula vary irregularly in brightness from gas jets off protostar

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22
Q

T Tauri Star

A

protostar about mass of Sun strong magnetic dynamo spinning fast, disk of material igniting of star and supernova push back on cloud and seed more stars in continuing cycle

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23
Q

Stellar Parallax (p)

A

small apparent shift in position of star against background due to Earth motion
half the apparent total shift of a star in photographs taken 6 months apart

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24
Q

Triangulation

A

finding distance by figuring out the distance to closer objects and triangulating
Stellar parallax is the larger version of this

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25
Q

Parsec (pc) (Parallax-arc-second)

A

astronomer choice, distance to object at parallax of 1 arc second, but because of atmosphere uncertainty

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26
Q

Absolute visual magnitude (Mv)

A

apparent visual magnitude if star were at standard distance of 33 ly away

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27
Q

Intrinsic brightness

A

measure of the amount of light a star produces

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28
Q

Flux

A

measure of energy flow from a surface
light in joules per second per meter squared
Also called watts

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29
Q

Luminosity (L)

A

total energy a star emits per second at all wavelengths

intrinsically brightest stars are -8 (almost as bright as Moon) emit 100 000 x more (visible) than Sun

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30
Q

Spectral class

A 
Star's grouping with other stars of similar appearing spectra defined temperature
each class divided into subclasses 0 to 9 get temperature to about 5%
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31
Q

Spectral Sequence

A

arrangement of spectral classes of stars from hot to cool

O B A F G K M, L T Y

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32
Q

Brown Dwarf

A

larger than Jupiter
heated by contraction and slowly cooling off
look dull orange or red (mostly infrared emitter)
L = warmer
T = cooler
Low luminosity

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33
Q

Hertzspring-Russel (H-R) Diagram

A 
plot of intrinsic brightness vs surface temperature of stars
absolute magnitude (surface area or luminosity) vs spectral class (temperature or colour)
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34
Q

Stefan-Boltzmann Law

A

luminosity controlled by temperature, cooler stars are fainter than hotter

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35
Q

Main Sequence

A

Upper left to lower right stars on HR Diagram, 90% of all normal stars, energy from nuclear fusion

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36
Q

Red Dwarf (lower main sequence)

A

less than .4 solar masses
pressure-temperature thermostat is low
consume H slowly
basically never die- most abundant star, completely convective from core to surface

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37
Q

Giant

A

10 to 100 x larger than Sun, cool but luminous, fusion

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38
Q

Super Giant

A

1000x Sun diameter, hot and luminous, generate energy by nuclear fusion

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39
Q

White dwarf

A

very hot, little surface so low luminosity, cooling

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40
Q

Luminosity Class

A

spectra line width group, larger star gas less dense so narrower width of spectral line

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41
Q

Mass-Luminosity Relation

A

collisions less often when gas is less dense, so mass is a main factor in determining luminosity
Luminosity is proportional to the mass to the 3.5 power
doesn’t work for giants, supergiants, and white dwarfs

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42
Q

Spectroscopic Parallax

A

estimate star distance by comparing spectral apparent to absolute magnitude

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43
Q

Binary Stars

A

pairs of stars orbiting each other, so far as hard to map orbit or so close appear as one
imaginary line connecting stars passes through the centre of massive, closer to the more massive star

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44
Q

Visual Binary System

A

separately visible binary stars in the telescope (more useful to astronomers)

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45
Q

Spectroscopic binary system

A

single point of light in a spectrum determined to be two stars
doppler shifted in opposite directions

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46
Q

Eclipsing Binary system

A

single light stars cross each other as seen from Earth, light curve regular dips

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47
Q

Light Curve

A

graph of brightness vs time (common for analysis of variable stars and eclipsing binaries
data often hard to analyze and requires a science process to resolve

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48
Q

Stellar Surveys

A

total star count estimated from a patch of sky
planning parameters and taking survey difficult to get fair/representative sample
M and white dwarves most common

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49
Q

Laws of Stellar Structure

A

1- conservation of mass- total mass = sum of shell masses
2- conservation of energy- total luminosity = sum energy generated in all layers in each shell
3- Hydrostatic equilibrium- weight of each layer balanced by the pressure in that layer (fluid balance)
4- energy transport- energy moves from hot to cool regions by conduction, radiation and convection

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50
Q

Conduction

A

close contact between atoms, less efficient, only rare stars with extremely high densities

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51
Q

Radiation

A

photons absorbed and re-emitted randomly to surface

depends on gas opacity (resistance to radiation flow), hot gas is more transparent, cooler opaque

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52
Q

Convection

A

back-up of photons heats gas that begins to rise, cooler settle, heat driven churn, motion

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53
Q

Stellar Model

A

table representing conditions in various layers of star, simulation possible

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54
Q

Mathematical Model

A

quantitative thinking, as good as theories and assumptions, check against reality with large and fast computers can be complex and many varied outcomes (views)

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55
Q

Star core

A

Sun/star make energy by breaking and reconnecting bonds between particles inside atomic nuclei

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56
Q

Burning

A

a process of breaking and reconnecting bonds between chemicals and/or elements

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57
Q

Nuclear Fission

A

split uranium nuclei into less massive fragments

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58
Q

Nuclear fusion

A

combine light nuclei of atoms into heavier (more massive nuclei)
products more tightly bound than the original nuclei, so energy is released

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59
Q

Coulomb Barrier

A

electrostatic force of repulsion between bodies (atomic particles) of like charge

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60
Q

Carbon-Nitrogen-Oxygen (CNO) Cycle

A

carbon as a catalyst to combine 4 hydrogen, produce energy in upper main sequence stars (more massive than Sun), a more efficient process

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61
Q

Proton-Proton Chain

A

series of three nuclear reactions, builds helium atom by adding together protons efficient in temperatures about 10 million K
two hydrogen combine nucleus (protons combine, one becomes neutron)

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62
Q

Deuterium

A

made in proton-proton chain

isotope of Hydrogen

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63
Q

Positron

A

antimatter electron emitted during proton-proton chain

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64
Q

Neutrino

A

neutral particle

emitted during proton-proton chain

65
Q

When stars are less massive than 0.08 solar masses, they…

A

cannot raise their central temperature and sustain hydrogen fusion

66
Q

Zero-Age Main Sequence (ZAMS)

A

stars first reach stability at the lower edge of HR diagram, they move above the line when they exhaust hydrogen

67
Q

Medium Mass (Sunlike) Star

A

less than about 4 solar masses

not hot enough to ignite carbon

68
Q

Yellow Giant

A

fusion reactions in the core, post main-sequence alive star, helium core fusion
on the horizontal branch

69
Q

Horizontal Branch (HR Diagram)

A

location of giant stars fusing helium

70
Q

Red Giant

A

fusion in core failing because of build up of C and O, dead star, losing mass

71
Q

Planetary Nebula

A 
expanding shell(s) of gas ejected from medium-mass dying star in red giant stage
explain by Kirchoff's laws and Doppler effect, slow winds and jets
72
Q

White Dwarf

A

remainder of central star contracts to dense core converting gravity to thermal energy

73
Q

Degenerate matter

A

extremely high density matter, pressure no longer depends on temperature
White Dwarves, etc

74
Q

Compact Object

A

does not generate nuclear energy, final stage, smaller denser than star but not a star

75
Q

Roche Lobe

A

volume of space a star sweeps gravitationally in a binary system

76
Q

Accretion Disk

A

rotating disk of matter forms as matter drawn gravitationally toward a central body

77
Q

Angular Momentum

A

measure of body to continue rotating, math product of mass, velocity and radius

78
Q

Nova

A

low mass super nova

79
Q

Type 1 A Super Nova

A

thermonuclear, white dwarf gains mass enough to exceed Chandresekhar-Landau limit

80
Q

Chandrasekhar-Landau Limit

A

greater than 1.4 solar masses, a star will not support itself and collapse to zero diameter

81
Q

Massive Star

A

upper main sequence

ignites fusion cells sequence

82
Q

Supergiant Star

A

fusion in core failing because of build up of elements to iron

83
Q

Supernova

A

exploding massive star, violent explosion, 4000x brighter than nova, long-lasting, rare

84
Q

Type II Supernova

A

massive star supernova completely explodes all but star core into space

85
Q

Supernova Remnant

A

nebulous remains, expanding shell of gas and dust exciting interstellar medium

86
Q

Neutron Star

A

small, highly dense star, radius about 10 km, almost entirely tight compacted neutrons

87
Q

Pulsar

A

source of regular, short, radio bursts, believed to be rapidly spinning neutron stars
discovered by Jocelyn Bell

88
Q

Millisecond Pulsar

A

fastest pulsars found, pulse period of only a few milliseconds

89
Q

Lighthouse Model

A

explains pulsar as neutron star spin sweeping beams of EM radiation

90
Q

Black hole

A

mass collapsed so small its gravity prevents all radiation from escaping a volume of space

91
Q

Singularity

A

a black hole

object of zero radius and density and gravity that are infinite

92
Q

General theory of relativity

A

Einstein’s 1916 theory

describes gravity as due to curve of space-time

93
Q

Space-time

A

space and time are related and can be considered together as the fabric of the universe

94
Q

Event horizon

A

edge, boundary of a black hold region where events are not visible to outside observer

95
Q

Schwarzschild Radius (Rs)

A

radius of a black hole event horizon, space-time folds back on itself

96
Q

Time dilation

A

slowing of moving clocks or clock in strong gravitational fields

97
Q

Gravitational redshift

A

lengthening of the wavelength of a photon as it escapes a gravitational field

98
Q

Gravitational radiation

A

rapid change in gravitational field transports energy outward at speed of light

99
Q

Hypernova

A

very massive star collapse into a black hole, possible source of focused gamma ray burst
star more than 15-20 solar masses would conserve angular momentum and sting rapidly, slowing at equator

100
Q

Gamma-ray burst

A

sudden powerful bust of gamma rays lasting seconds then fading, discovered in 1960’s

101
Q

Galaxy

A

William and Caroline Herschel published it as a star system

“milk”

102
Q

Cepheid variable stars

A

have a pulsation period of 1-60 days related to luminosity

Henrietta Leavitt identified link of pulsating stars and their distance related to power

103
Q

Instability strip

A

Cepheid variable stars pass through here

temperature and luminosity where stars are unstable therefore they puslate

104
Q

Period-luminosity relation

A

between period of pulsation and intrinsic brightness Cepheid variable
Harlow Shapley noted open star clusters concentrated along Milky Way, globular scattered, using cepheid variable to calculate distances

105
Q

Proper motion

A

arc second/year/rate star moves
replaces Leavitt’s apparent magnitude with absolute magnitude
calibrated the variable stars for distance

106
Q

Calibration

A

in science, carefully taken measures and background work for others to use important to get calibration right because it could throw off many following measurements

107
Q

Disk Components

A

all matter confined to plane of rotation of a galaxy (stars, open clusters, gas, dust)
gas and dust block view in optical wavelengths, full view in near infrared and far-infrared views

108
Q

Disk

A

contains lots of gas, site of most star formation, lit by recently formed blue stars

109
Q

Galactic Plane

A

stars more in a similar direction in nearly circular orbits in this area

110
Q

Spiral Arms

A

long curves from centre to edge of bright stars, star clusters, gas, dust (star formation)
a pattern in disk (not structures and not connected)

111
Q

Spiral Tracers

A

map spiral arms by association
OB stars
open clusters, ionize H clouds, variable stars

112
Q

Density wave theory

A

arm formation as compressions of the interstellar medium in the disk of galaxy
gas cloud overtake slower moving density wave, compressed in traffic jam, eventually move on

113
Q

Two Armed grand spiral pattern galaxy

A

only a spiral density wave can produce this pattern

114
Q

Self-Sustaining Star formation

A

luminosity burst, jets from newborn stars or novae trigger more stars
differential rotation can drag region inner edge ahead producing cloud of star formation spiral arm

115
Q

Spherical Component

A

matter scattered in roughly spherical distribution around central point
a ‘fossil’ because halo stars formed when galaxy young

116
Q

Halo

A

spherical region of spiral galaxy, thin scattering of stars, 2% as many as disk, very little gas/dust
no raw material, so mostly old stars, cool giants or dim lower-main sequence, old white dwarfs
randomly tipped orbits to the galactic plane

117
Q

Central Bulge

A

dense cloud of stars that surrounds centre of galaxy, old cool stars, redder, little dust
can also be an elongated bar, perhaps Milky Way

118
Q

Rotation Curve

A

graph, orbital velocity vs radius in disk of galaxy

119
Q

Keplerian motion

A

expected (3rd law) orbital velocity high near centre mass, falls off (by Sun)
curve is flat, past sun, not decrease for spiral galaxy, suggesting sifniciant mass outside sun may increase at greater distance, large amount of matter beyond the expected limit

120
Q

Dark Halo

A

low-density extension of halo, composed of dark matter, most not producing light, halo is older than the disk

121
Q

Dark Matter

A

nonluminous matter suggested by its gravitational influence

122
Q

Population I stars

A

rich in metals, located in the disk

123
Q

Metal

A

all atoms heavier than helium

124
Q

Disk Populations stars

A

2-3% heavier than helium

circular orbits in galactic plane, young

125
Q

Population II stars

A

poor in metals, located in halo, globular clusters, central bulge

126
Q

Monolithic collapse model

A

1950’s hypothesis galaxies formed from collapse of a single large cloud
outdated

127
Q

Bottom up hypothesis

A

more recent, galaxies built by cannibalizations (accumulation) of others

128
Q

Nucleus

A

very centre of galaxy, visual wavelengths is totally hidden by gas, dust, dim light 30 magnitudes

129
Q

Sagittarius A Star, Sgr A*

A

intense radio source at centre of Milky Way Galaxy

only a few astronomical units in dimeter, crowded stars and dust warmed by those stars

130
Q

Milky Way Galaxy Nucleus

A

4.6 million solar masses black hole

probably formed as the galaxy took shape

131
Q

Galaxy classification system

A

designed by Edwin Hubble, 1920’s

range in size rom dwarf to huge giants

132
Q

Elliptical Galaxy (E)

A

round or elliptical, no visible gas- dust, few or no bright stars

133
Q

Spiral Galaxy (S)

A

about 35% disk, spiral arm, halo stars not visible, gas, dust, hot O and B stars (new forming)

134
Q

Barred Spiral Galaxy (SB)

A

2/3 of spirals, elongated nucleus, bar of elliptical orbit stars/gas, spiral arms

135
Q

Irregular Galaxy (Irr)

A

25% of all galaxies, no obvious bulge/arms, chaotic mix of gas, dust, stars, dramatic star birth

136
Q

Small Magellanic Cloud

A

southern sky passing near ours, interacting gravitationally with Milky Way

137
Q

Large Magellanic Cloud

A

Southern sky, Tarantula Nebula, an interacting neighbour as well

138
Q

Distance ladder

A

calibration to build a distance scale from Earth size to most distant galaxy
rests on understanding of luminosity of stars, ultimately back to stellar parallax
distance to galaxies astronomy use megaparsec (Mpc)

139
Q

Standard candles

A

common objects of known brightness to estimate distance

Cepheid Variable, novae

140
Q

Tully-Fisher Relationship

A

linear relationship between luminosity and rotational rate of spiral galaxies to determine distance to spiral galaxy as a standard candle

141
Q

Look-back time

A

time in years equal to the distance to the object in light years
Moon only 1.3 seconds, Sun 8 minus, neared star 4Y, andromeda 2 million years

142
Q

Hubble’s Law

A

linear relation between distance to galaxy and apparent velocity of recession (expansion)
1929 published graph because lines in galaxy spectra are generally shifted toward longer wavelengths

143
Q

Hubble Constant

A

universe expansion rate, slope of apparent recession velocity against distance important as evidence universe is expanding and redshift can estimate distance

144
Q

Rotation Curve Method

A

determine galaxy’s mass by observing orbital velocity and orbital radius to stars only galaxies near enough to be well resolved visually, Kepler’s third law finds the mass within the orbit

145
Q

Rich Galaxy Clusters

A

over 1000 or more, mostly elliptical, in a volume only a few Mpc in diameter
with one or more giant elliptical galaxies at the center

146
Q

Poor Galaxy clusters

A

irregular shape cluster of fewer than 1000 many spiral, no giant ellipticals less crowded towards the centre

147
Q

Gravitational Lensing

A

curving of light by a large mass (multiple images of the source can be seen)
gravitational effect a cluster has on light from more distant objects, used to estimate galaxy mass

148
Q

Tidal Force

A

mass of one galaxy to distort or rip apart another galaxy, can stimulate spiral arm formation

149
Q

Tidal Tails

A

long streamers of stars and material that connect galaxies as they pass by each other

150
Q

Ring Galaxy

A

resemble ring around bright nucleus, collision of two galaxies, wave of star formation, spiral around common center

151
Q

Shell of Stars

A

tides rip stars away from a ring galaxy to form this shell

152
Q

Starburst Galaxies

A

very luminous in infrared because undergoing star formation

153
Q

Quasar (Quasi-Stellar Object, QSO)

A

extreme small active galactic nucleus of very distant galaxy

154
Q

Active Galaxy

A

high energy sources in nuclei, black hole, emit excess energy as jets, outbursts, radio

155
Q

Radio Galaxy

A

discovered in 1950’s, strong source of radio signal
1970’s, see bright at other wavelengths
emit large amounts of excess energy at Active Galactic Nuclei

156
Q

Seyfert Galaxy

A

otherwise typical but with unusually luminous small core that fluctuates in brightness
suspected result of collision with companion, large central mass holds gas jet from escaping

157
Q

Double Lobed Radio Source

A

emit radio energy from two regions (lobes) opposite sides of galaxy
1950’s identified pairs of radio-bright regions, later observation confirmed galaxy between jet
compact by intense magnetism and highly energized particles

158
Q

Blazar

A

view into central cavity can see blazar

very luminous highly variable source (few/no emission lines)

159
Q

Unified Model

A

explains many active galactic nuclei using single model viewed from different directions

SC120 (2 decks)

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