Download - Method of Trigonometric Parallaxes
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Method of Trigonometric Parallaxes
June
December
Distant Stars
ForegroundStar
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Closer stars have larger parallaxes:
Distant stars have smaller parallaxes:
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Sun
Sun No propermotion
Large propermotion
Proper Motions
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1902
1952
2002
Barnard’s Star
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Case Study: The Big Dipper
Today
50,000 BC
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50,000 BC
Today
50,000 AD
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No Shift
Blueshift Redshift
Radial Velocities
Sun
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Space Velocity
Sun
TangentialVelocity
Radial Velocity
Proper Motion (angle)
Distance
2t
2r
2 vvv
tv 4.74 d=
SpaceVelocity
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d=1
d=2
d=3
B=1
B=1/9
B=1/4
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Center of Mass
M2
M1
a
a1a2
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A
A
B
B
B
A
A
B
Spectroscopic Binary
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Eclipsing Binary
Time
3
1
Brig
htne
ss
4
2
1
3
2
4
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Hydrogen
Continuum
Absorption Lines
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The Spectral Sequence
Bluest Reddest
Spectral Sequence is a Temperature Sequence
Hottest Coolest50,000K 1300K
O B A F G K M L
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H–R Diagram
40,000 20,000 10,000 5,000 2,500
106
104
102
1
102
104
Temperature (K)
Lum
inos
ity (L
sun)
White Dwarfs
Giants
Supergiants
Main Sequence
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Russell (1912) HIPPARCOS (1999)
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HipparcosH-R Diagram
4902 single starswith distance errors of <5%
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L M4
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Hydrostatic Equilibrium
Gas Pressure
Gravity
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Core-Envelope Structure
Hot, Compact Core
Cooler,ExtendedEnvelope
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Photon Random Walk
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Convection
cooler watersinks
Hot blob rises
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Proton-Proton Chain:
(twice) eHpp e2
(twice) HepH 32 ppHeHeHe 433
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positron
neutrino
2H
positron
neutrino
2Hphoton
3He
4He
photon
3He
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CNO Cycle:12C + p N
N C e
C p N
N p O
O N e
N p C He
e
e
13
13 13
13 14
14 15
15 15
15 12 4
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Main Sequence
40,000 20,000 10,000 5,000 2,500
106
104
102
1
10-2
10-4
Temperature (K)
Lum
inos
ity (L
sun)
HighMass
LowMass
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Upper Main Sequence Star
RadiativeEnvelope
ConvectiveCore
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ConvectiveEnvelope
RadiativeCore
Lower Main Sequence Star
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ConvectiveEnvelope
ConvectiveCore
Red Dwarf Star
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20,000 10,000 5000 2500Temperature
105
103
102
0.1
0.01
104
10
1
Lum
inos
ity
(Lsu
n)
15 Msun
5 Msun
2 Msun
1 Msun
0.5 Msun
Zero-Age Main Sequence
Pre-Main Sequence Evolution
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Red Giant Star
InertHe
Core
H BurningShell
Cool, ExtendedEnvelope
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Climbing the Red Giant Branch
40,000 20,000 10,000 5,000 2,500
106
104
102
1
10 -2
10 -4
Temperature (K)
Lum
inos
ity (L
sun) Main Sequence
H-core exhaustion
Red GiantBranch
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Horizontal Branch Star
HeBurning
Core
H BurningShell
Envelope
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Horizontal Branch
40,000 20,000 10,000 5,000 2,500
106
104
102
1
10 -2
10 -4
Temperature (K)
Lum
inos
ity (L
sun) Main Sequence
H-core exhaustion
Red GiantBranchHorizontal Branch
HeliumFlash
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Asymptotic Giant Branch Star
InertC-OCore
He BurningShell Cool, Extended
Envelope
H BurningShell
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The Asymptotic Giant Branch
40,000 20,000 10,000 5,000 2,500
106
104
102
1
10 -2
10 -4
Temperature (K)
Lum
inos
ity (L
sun) Main Sequence
H-core exhaustion
Red GiantBranchHorizontal Branch
AsymptoticGiant Branch
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Planetary Nebula Phase
40,000 20,000 10,000 5,000 2,500
106
104
102
1
10 -2
10 -4
Temperature (K)
Lum
inos
ity (L
sun)
Main Sequence
Bare Core
WhiteDwarf
Envelope Ejection
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Red Supergiant Star
InertHe
Core
H BurningShell
Cool, ExtendedEnvelope
Not to Scale
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Supergiant Branch
40,000 20,000 10,000 5,000 2,500
106
104
102
1
10 -2
10 -4
Temperature (K)
Lum
inos
ity (L
sun)
RedSupergiant
Main Sequence
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Blue Supergiant
40,000 20,000 10,000 5,000 2,500
106
104
102
1
10 -2
10 -4
Temperature (K)
Lum
inos
ity (L
sun)
Blue Supergiant
HeliumFlash
Main Sequence
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End of Helium Burning
40,000 20,000 10,000 5,000 2,500
106
104
102
1
10 -2
10 -4
Temperature (K)
Lum
inos
ity (L
sun)
Main Sequence
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End of Carbon Burning Phase
InertO-Ne-Mg
Core
C BurningShell
Red SupergiantEnvelope
He BurningShell
H BurningShell
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End of the Silicon Burning Phase
InertFe-NiCore
Si BurningShell
O BurningShell
Ne BurningShell
C BurningShell
He BurningShell
H BurningShell
Envelope Radius: ~ 5 AU
Core Radius: ~1 Rearth
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Crab NebulaRemnant of Supernova in 1054 AD
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40,000 20,000 10,000 5,000 2,500
106
104
102
1
10-2
10-4
Temperature (K)
Lum
inos
ity (L
sun)
Age: ~1 Myr
Zero AgeMain Sequence
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40,000 20,000 10,000 5,000 2,500
106
104
102
1
10-2
10-4
Temperature (K)
Lum
inos
ity (L
sun)
Age: ~10 Myr
B Stars
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40,000 20,000 10,000 5,000 2,500
106
104
102
1
10-2
10-4
Temperature (K)
Lum
inos
ity (L
sun)
Age: ~100 Myr
A Stars
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40,000 20,000 10,000 5,000 2,500
106
104
102
1
10-2
10-4
Temperature (K)
Lum
inos
ity (L
sun)
Age: ~1 Gyr
F Stars
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40,000 20,000 10,000 5,000 2,500
106
104
102
1
10-2
10-4
Temperature (K)
Lum
inos
ity (L
sun)
Age: ~10 Gyr
G Stars
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Age: ~10 Myr Age: ~1 Gyr
TempBlue Red Temp
BStars
FStars
Lum
inos
ity
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Typical Globular Cluster H-R Diagram
40,000 20,000 10,000 5,000 2,500
106
104
102
1
10-2
10-4
Temperature (K)
Lum
inos
ity (L
sun)
HorizontalBranchZero-Age
MainSequence Giant
Branch
MainSequence
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Sirius BM 1.0 Msun
R 5800 km
White Dwarf
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Neutron Star
M=1.5 Msun
R10 km(spaceimaging.com)
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Inside a Neutron Star
CrystallineIron Crust
NeutronSuperfluid
??
SuperconductingProtons
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RadiationBeam
MagneticField
SpinAxis
Pulsar Model
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Neutron Star vs. Black Hole
Neutron StarM=1.5 Msun
R=10 kmManhattan
(spaceimaging.com)
Black HoleM=1.5 Msun
RS=4.5 km
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Jack
Jill
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Spectroscopic Parallax
A8V Star
40,000 20,000 10,000 5,000 2,500
106
104
102
1
10-2
10-4
Temperature (K)
Lum
inos
ity (L
sun)
A8I Star
L = 10 Lsun
Spectral Type
L = 22,000 Lsun
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Period-Luminosity Relationship
1 5 10 50
102
103
104
Period (days)
Lum
inos
ity
(Lsu
n) Cepheids
RR Lyraes
3 100300.5
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Cepheid P-L Relation
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Example: Cepheid with a 10-day period
1 5 10 50
102
103
104
Period (days)
Lum
inos
ity
(Lsu
n)
3 100300.5
L=5011 Lsun
P=10d
CepheidP-L Relation
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Wright’s Milky Way (1750)
Manystars
Few Stars
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The Herschels’ Milky Way Map (1785)
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Kapteyn Model (1922)
~17 kpc
~3 kpc
kpc = kiloparsec = 1000 pc
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Shapley’s Globular Cluster Distribution
3020101020 40
10
20
10
20
kpc
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Hubble “Tuning Fork” Diagram
E0 E3 E7
SBa SBb SBc
Sa Sb Sc
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NGC 4414Type Sc
Flocculent & Grand Design Spirals
NGC 628Type Sc
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E1 E5
Elliptical Galaxies
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Sa
Sb
Sc
Ordinary Spirals
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SBa
SBb
SBc
Barred Spirals
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Irregular Galaxies
Large Magellanic Cloud Small Magellanic Cloud
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NGC 628Face-On Sc
NGC 891Edge-On Sb
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Rotating Disk
Rotation Axis
Approaching SideBLUESHIFT
Receding SideREDSHIFT
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Differential Rotation
Inner orbit pulls ahead
Outer orbitlags behind
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Schematic Spiral Galaxy Rotation Curve
0
0
25
200
100
5 10 15 20
Radius from the Center (kpc)
Rot
atio
n S
peed
(k
m/s
ec)
Solid-BodyRotation
Differential Rotation
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Observed vs. Predicted Keplerian
50
200
100
0
10 20 30 400Radius from the Center (kpc)
Rot
atio
n S
peed
(k
m/s
ec)
KeplerianPrediction
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Orbit Crowding Schematic
Nested EllipticalOrbits, each oneslightly rotated.
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NGC147NGC185
M32
And IIAnd III
Fornax
Scupltor SMC
Sagitarius
DracoUrsa Minor Leo II
NGC 205And I
NGC 6822
M31
M33
IC1613
LMC
MW
Carina
Leo I
The Local Group
1 Mpc
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~100 Mpc
Local Group
LocalSupercluster
Data from Tully, 1982, ApJ, 257, 389
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Voids
Filaments2dF Redshift Survey>120,000 Galaxies
300 Mpc
600 Mpc
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Raising Tides
Far side Near side
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Bright Active Galaxy
NGC 5548
Variability (1988-1996)HST Image
OSU AGN Watch
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Normal Galaxy
Active Galaxy
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Composite Quasar SpectrumSloan Digital Sky Survey
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Jane’s clock as seen by Jane:
Tick!!
Photon Path = 3 meters
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Jane’s clock as seen by Dick:
0.8c
Tick!!
Photon Path = 5 meters
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Perihelion Precession of Mercury
Earlier Later
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Bending of Starlight(side view)
TruePosition
Sun
ApparentPosition
Scale is exaggerated
Earth
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0 0.5 1Deflection(arcsec)
1o 2o
1o
2oView from EarthData from 1922 Eclipse
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Hubble’s Data (1929)
1000
500
0
0 1 2Distance (Mpc)
Rec
essi
on V
eloc
ity
(km
/sec
)
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Hubble & Humason (1931)
10 20 30
5000
10,000
15,000
20,000
Rec
essi
on V
eloc
ity
(km
/sec
)
Distance (Mpc)
1929 Data
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Freedman et al. (2001) – HST Key Project
Freedman et al. 2001, ApJ, 553, 47
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Freedman et al. 2001, ApJ, 553, 47
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Expanding Space-Time
Universe 2x largerGalaxies are 2x further apart
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Recession Velocity (cz)
Dis
tanc
e (d
)
Accelerating(slower in past)
Decelerating(faster in past)
Constant
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2-D Examples of Curved Spaces
Positive(Spherical)
Flat
Negative(Hyperbolic)
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d L (d
ista
nce)
Dev
iatio
n fro
m
=0
, m=0
.3 m
odel
Redshift (z)
m=0.3, =0
Accelerated
Decelerated
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Very Open<<1
Closed>1 Oscillating?
Time
Dis
tanc
e B
etw
een
Gal
axie
s
~100 Billion Years
Histories for =0
Critical/Open=1
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Matter & Energy Content of the Universe
dm
m
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Size
Binding Energy
Atoms 10–10 m 103 K Nuclei 10–14 m 1010 K p & n 10–15 m 1011 K Quarks 10–18 m 1013 K
Typical Sizes & Binding Energies
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Big
Ban
g
Infla
tion
GU
Ts E
poch
Pla
nck
Epo
ch
Nuc
leos
ynth
esis
Nuc
leon
Fre
ezeo
ut
Qua
rk F
reez
eout
Ele
ctro
wea
k D
ecou
plin
g
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Rec
ombi
natio
n30
0,00
0 yr
Toda
y~1
3 G
yr
Dar
k A
ges
Firs
t Sta
rs &
G
alax
ies
1 G
yr
500
Myr
Big
Ban
g0
Sun
For
ms
9 G
yr