lab 11
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Astronomy 105 Laboratory. Lab 11. Lab Quiz 11. Hubble discovered that galaxies are moving away from the Milky Way with velocities that are proportional to their . size. color. distance. mass. - PowerPoint PPT PresentationTRANSCRIPT
LAB 11Astronomy 105 Laboratory
LAB QUIZ 11
Hubble discovered that galaxies are moving away from the Milky Way with velocities that are proportional to their
1. size.2. color.3. distance.4. mass.
Consider two galaxies which are different distances from the Milky Way. One galaxy is 10 Mly distance and the other 30 Mly. How much larger or smaller is the recessional velocity of the more distant galaxy? 1. 3 times larger
2. 6 times larger3. 9 times larger4. 3 times smaller5. 6 times smaller6. 9 times smaller
Consider two galaxies that are the same size but one is twice as far away as the other. The more distant galaxy will have ____ compared to the closer galaxy. 1. ½ the angular size
2. ¼ the angular size3. 2 times the angular size4. 4 times the angular size
In today’s lab you will determine the rotation rate of the planet Saturn by using
1. Hubble’s Law.2. Newton’s Law of Gravity.3. the Doppler Effect.4. the luminosity-distance formula.5. the distance modulus.
AST 105 Review for Lab Exam
Exam Next Week!
Study!
About 3-5 questions from each lab exercise Review
Main concepts covered Procedures and measurements Questions and calculations Bring a scantron: 882-E Review material – Power point slides online
EXPERIMENTAL MEASUREMENTS
Scientific Experiments / Observations
Physical quantities can never be measured with absolute precision
How Many Significant Figures0.089 2
1.089 4
12000 2
12001 5
Scientific Notation
3.502 x 106
decimal number (1-9)10 raised to an integer power
Number Significant Figures Scientific Notation
9004 4 9.004 x 103
0.000007 1 7 x 10-6
43 2 4.3 x 101
7,805,000,000 4 7.805 x 109
0.0408 3 4.08 x 10-2
8.4 2 8.4 x 100
To multiply two numbers in scientific notation multiply the decimal parts of the numbers and add the exponents algebraically.
(4.0 x 104)(2.0 x 103) =(4.0 x 2.0)(104 x 103) =(8.0) x (104+3) =8.0 x 107
(6.0 x 102)(2.0 x 105) = 12.0 x 107 = 1.2 x 108
CONSTELLATIONS – SKY FAMILIARIZATION
North
South
Celestial Equator
Ecliptic Sun’s Path
East
Summer Solstice
Vernal Equinox
Autumnal Equinox
North
South
East
March 7 @ 8:00 p.m
Meridian
Zenith
32° X
West Horizon
March 7 @ 8:00 p.m
Meridian
not visible
WestEast
East HorizonWest Horizon
Sky Familiarization
A Few More Things to Remember Any vertical line on your SC-1 (north-south) is a
meridian. Approximately one half of the stars on the SC-1
are visible at any given time (12 hours of RA). Meridian moves eastward 4 minutes each day
(Earth’s revolution) Meridian moves eastward 1 hour of RA for every
hour of time (Earth’s rotation)
THE MOON
N.P.N.P. N.P.
N.P.
N.P.
Synchronous Rotation
Does the Moon rotate on it’s axis?
What is the Moon’s hidden side?
N.P. Noon
Sunset
Midnight
Sunrise
N.P. Noon
Sunset
Midnight
Sunrise
N.P. Phase: 1st quarter
Rise Time:
Set Time:
Transit:
Noon
Midnight
Sunset
MERCURY’S ORBIT
10 20 30 40 50 60 70 80 90 100010 km6
SUN
Name (print):__________________________________ Section: _____
0.70.60.50.40.30.20.10.0AU
0.8
110 120
Mercury’s Orbit
Major Axis
Equal Time Intervals
F F
Verifying Kepler’s 1st
Mercury’s Orbit
Major Axis
10 20 30 40 50 60 70 80 90 100010 km6
SUN
0.70.60.50.40.30.20.10.0AU
0.8
110 120
Verifying Kepler’s 2nd
Equal area in equal time.
Mma
G4πP
322
2
324Pa
GMm sunm
sunsunm MMm
Kepler’s 3rd
)(4 2
MmGk
2
324Pa
GM sun
Finding the Sun’s mass.
P2=ka3
EMISSION SPECTRA
Formation of Emission and Dark Line Spectra
THE EARTH’S ORBITAL VELOCITY
12
345
Velocity = 0
Increasing Velocity
Increasing Velocity
The Doppler Effect
or
cv
Arcturus
VA
VB
? ?
0A λ
Δλcv
o
From measured Doppler Shift1.Orbital velocity of Earth
2.Radial velocity of Arcturus
3.Radius of the Earth’s Orbit
THE HR DIAGRAM
Apparent Brightness of Stars
Stellar Luminosity -- Total amount of light energy emitted each second Surface Area Temperature
Distance from the Earth
Magnitude
Stellar Brightness Apparent Magnitude (mv) - Brightness from Earth Absolute Magnitude (Mv) - Brightness from 10 pc
Absolute magnitude depends only on a star’s luminosity (the star’s wattage)Magnitude Difference
Brightness Ratio (Brightness Difference)
1 (2.512)1 2.5 2 (2.512)2 6.3 3 (2.512)3 15.9 4 (2.512)4 40 5 (2.512)5 100 6 (2.512)6 251
Spectral Classification
B
The SunM=+5 G2
O B A F G K M
-10-5 0+5+10+15A
bsol
ute
Mag
nitu
de
Temperature
HR Diagram
Luminosity Class
Size
Ia & Ib Supergiant
II Bright Giant
III Giant
IV Sub-giant
V Dwarf
The Sun’s Spectral and Luminosity Class: G2 V
Star mv Mv
SpectralType
LuminosityClass
Aldebaran +0.9 -0.2 K5 IIIAlpha Centauri A 0.0 +4.4 G2 V
Antares +0.9 -4.5 M1 ICanopus -0.7 -3.1 F0 II
Fomalhaut +1.2 +2.0 A3 VRegulus +1.4 -0.6 B7 V
Sirius -1.4 +1.4 A1 VSpica +0.9 -3.6 B1 V
Which star appears faintest in our sky? Regulus
Which star has the greatest luminosity? Which star has the highest surface temperature? Which star is a red giant?
Which main-sequence star has the longest lifetime?
Antares
Spica
Aldebaran
Alpha Centauri
THE DISTANCE TO THE PLEIADES
Stars in a Cluster• Common Properties
• Distance• Age
• Different Properties• Spectral Types (temperature)• Luminosity Class (size)
d >10 pc
10 pc
d <10 pc
10 pc
Star Cluster
d >10 pc
d <10 pc
O B A F G K M-0.4 color index 1.3
Main-sequence
HR Diagram
-0.4 color index 1.3
Color-MagnitudeDiagram
Distance Modulus = m - M The difference between the absolute magnitude and the apparent magnitude can be used to find the distance to a star cluster. If m-M > 0 then the distance to the cluster is > 10 pc.If m-M = 0 then the distance to the cluster is = 10 pc.If m-M < 0 then the distance to the cluster is < 10 pc.
DM{
Cluster A: Distance 50 ly
Cluster B: Distance ?
The apparent brightness of the stars in Cluster B are 4 times fainter than the stars in Cluster A.
What is the distance to Cluster B?
Inverse-Square Law: √4 = 2
Cluster B is 2 times farther or 100 ly.
AGES AND DISTANCES TO CLUSTERS
Interstellar Dust Reddens Light (makes stars appear cooler) Dims Light (makes stars appear further away)
age of cluster = lifetime of stars at main-sequence turnoff point
B6 stars -- 60 million yrs. MS lifetime
Pleiades - Open Cluster
Distance - 380 ly Age - 60 million years
HUBBLE’S LAB
V = 0 2800210014007007001400km/sec
10 Mpc 20 Mpc 30 Mpc 40 MpcMilky Way A B C
V = 02800 2100 14007007001400km/sec
10 Mpc 20 Mpc30 Mpc40 MpcMilky Way A B C
10 Mpc20 Mpc Alien’s Galaxy
Recessional Velocity is Proportional to Distance
The Universe is Expanding!!
v = Ho dHubble Diagram
Finding a Galaxy’s Distance Hubble’s
Law
d = v / Ho
To Find Distance: Measure recessional velocity (red shift)
132 Mpc
Sample Galaxies
Distance images
Recessional Velocity spectra
v = Ho x dHubble Diagram
Hubble Diagram
Procedure- plot data- draw best fit line- find slope (Ho)x
x
x
xx
rise
run slope = rise/run
ROTATION OF SATURN
Earth Distant Star
Laboratory - No Radial motion
Radial Velocity = 0
Radial Velocity -
Radial Velocity +
Laboratory Spectrum
Blueshift
Redshift
Spectral Lines Match
o
Important: Do not write or mark on the
Saturn Handout
Spectroscope Slit
No Doppler Shift from this Light
Light from here shows the largest Blue Shift
Light from here shows the largest Red Shift
A
BSaturncV
λΔλ 0B 2
o A
B
seckm
04λΔλcV
V
V
0λΔλcV Doppler
cV
λΔλ 0A 2
o
seckm
04λΔλcV
Top
Bottom
(mm) = Top Distance – Bottom Distance
Reference Line
c = 300,000 km/s
o = 6200 Å
Finding the Rotation Period of Saturn
Saturn
V Period = Distance / Velocity
Distance = Equatorial Circumference = 2RR
P = 2 R / V
VR2P
Period (P) – Rotation Period
THE END
5 pc 10 pc 15 pc-26.5
1.3
3.3
2.0
4.2
Sun
A
B
C
D
5.06.0
0.0
2.0
Apparent Magnitude
Absolute Magnitude
1 parsec (pc) = 3.26 ly
Verifying Kepler’s 2nd
Equal area in equal time.
A2
A1
base
periluna
Center
Verifying Kepler’s 1st
P1L1
L2
P2
L3
L4
The AST105 Lab Exam is the week of November 29 (Week after Thanksgiving).1. True2. False
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