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CENTRAL TEXAS COLLEGE
SYLLABUS FOR PHYS 1403
STARS and GALAXIES
Semester Hours Credit: 4
INSTRUCTOR:
OFFICE HOURS:
I.
INTRODUCTION
A.
Stars and Galaxies is one of the two introductory Astronomy classes we teach here
at Central Texas College. The other class is what we call Solar System.
Astronomy was the first of the sciences, and when colleges and universities were
established in the middle Ages, it was one of the seven subjects taught to all
students. It has always had important applications, including calendar making,
time keeping, and navigation. Nowadays, astronomy is adding other practical
applications, such as addressing vital questions about climate change on Earth. It
is further expanding our knowledge of the solar system and space, where there are
potentially unlimited supplies of energy and materials. Over the coming decades
and centuries, new resources can begin to free mankind forever from speculation
or belief about their position in this universe.
B.
But the main job of this class is simply the advancement of knowledge. It will
provide a sense of the mystery and majesty of the universe. As with our ancestors
back beyond recorded time, we can’t help but wonder what kind of Universe is
this? What are its fundamental laws? How old is it? How big? What does it
contain? How has it changed with time, and what may be its future? We now
know a great many answers, but behind every curtain of the unknown lay another
question, or several.
C.
Every part of astronomy, from planets to black holes, has its mysteries.
Astronomers are working on these things. Such pure research is one of the most
important human activities. This is only partly because unexpected discoveries
and new insights often lead to the biggest payoffs. More importantly, if we ever
lose our sense of wonder, and stop trying to understand, the lights will be going
out for the human race.
This course may be used as an elective in many programs, and may also fulfill the science
requirement for a degree plan in many programs. It is the duty of the student to ascertain whether
this course will properly transfer to that student’s targeted university or college.
D.
8/29/11
Themes of the Course
1.
2.
3.
4.
5.
6.
7.
8.
II.
The Universe is dynamic and continually evolving.
The universality of physical laws discovered on Earth allows us to analyze
and draw conclusions about celestial phenomena that can be studied only
at great distances.
Scientific conclusions must be based on an exacting comparison of
hypotheses to evidence obtained from observations and experimental data.
The Universe, because it has objects and environments that cannot be
duplicated on Earth, is a unique laboratory for testing scientific
hypotheses.
Because astronomy is a human endeavor, it is subject to both the
limitations and the enhancements of personal relationships, biases,
inspiration, and creativity.
Most astronomical knowledge accumulates incrementally, with each new
piece of knowledge providing a potential foundation for further
understanding.
Observational and computational technologies play critical roles in
shaping our understanding of the Universe.
In addition to scientific value, astronomy has practical and philosophical
value because humans are participants in, as well as observers, of the
universe.
LEARNING OUTCOMES
Upon successful completion of this course, PHYS 1403, Stars and Galaxies, the student
will be able to:
A.
Describe the electromagnetic spectrum and explain the purposes of the different
types of observing techniques and instruments used in astronomy.
B.
Explain the significance of the appearance of astronomical objects seen in the sky,
describe celestial positions, and explain the working of time zones and calendars.
C.
Recognize major constellations, stars, star groups, features on the moon and planets
when seen in the sky.
D.
Describe the general characteristics of the various kinds and ages of stars, and explain
how they generate energy.
E.
Discuss the life cycles of stars.
F.
G.
Explain the types, components of galaxies and describe their evolution.
Discuss the origins and evolution of the universe.
PHYS 1403
2
III.
H.
Demonstrate competence in using a telescope.
I.
Demonstrate the ability to read and interpret astronomical diagrams, charts, graphs,
tables, and models (both mental and physical).
J.
Show greater understanding and appreciation for the history, nature, and methods of
science and astronomy.
K.
Show positive attitudinal changes regarding astronomy and science in general.
L.
Demonstrate increased ability to critically think when presented with astronomical
problems and situations.
INSTRUCTIONAL MATERIAL
A.
The instructional materials identified for this course are viewable through
www.ctcd.edu/books
B.
REQUIRED LABORATORY BOOK: Twenty-one Activities concerning “Where
We Are in Space and Time”, Project STAR, The Harvard-Smithsonian Center
for Astrophysics, 1990. If you have already taken PHYS – 1404, (Solar System)
then your lab will consist of computer activities from “Starry Night Pro Activities
& Observation and Research Projects”. This is in the text book bundle. Also there
will be a number of labs involving hands-on activities. Your instructor will
provide the hand-outs on how to do those activities.
A scientific calculator.
Experimental Research Notebook (Optional).
C.
D.
IV.
COURSE REQUIREMENTS
A.
Your primary responsibility is to function as a college student, interested in
putting forth the effort required to obtain a passing grade in Stars and Galaxies.
You are to put into use all of your learning skills, acquired from past and present
educational experiences, in order to carry out this requirement.
B.
You may well find it useful and advantageous to answer the end-of-chapter questions
which you will find useful in guiding your review of the reading and video program. Your
answers to these discussion questions probably will not be collected (depending on the
requirements of your instructor/mentor/proctor), but will form part of your study guide.
C.
Each part of the course is not self-contained. You may expect that basic concepts
presented at the beginning of the course will be built upon day by day, added to,
expanded upon, etc., so that with time you will have both specific and overall
understandings. It is important to link together each piece in an attempt to achieve
PHYS 1403
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the comprehensive realization.
V.
D.
You are expected to maintain good class notes, since any material given in the text
and video programs may be included on exams. Pay particular attention to those
items that are stressed or emphasized.
E.
Regular class attendance is essential for passing the course. Excessive un-excused
absences will result in you being dropped from the course with a grade of “F”.
See Section VII below for further information.
EXAMINATIONS
There will be four unit exams given at the times announced. Lowest exam score will be
dropped. Missed exams will not be made up under any circumstance. There will also be a
comprehensive final exam. The final exam cannot be missed.
VI.
SEMESTER GRADE COMPUTATION
Hour exams
Final exam
Quizzes
Home work
Planetarium & Observations
Laboratory
Total
VII.
40%
10%
10%
10%
10%
20%
100%
90% - 100% = A
80% - 89% = B
70% - 79% = C
60% - 69% = D
0% - 59% = F
NOTES AND ADDITIONAL INSTRUCTIONS FROM COURSE INSTRUCTOR
A.
Withdrawal from the course: It is the student’s responsibility to officially drop a
class if circumstances prevent attendance. Any student who desires to, or must,
officially withdraw from a course after the first scheduled class meeting must file
an Applications for Withdrawal or an Application for Refund. The withdrawal
form must be signed by the student. Application for Withdrawal will be accepted
at any time prior to Friday of the 12th week of classes during the 16 week fall and
spring semesters. The deadline for sessions of other lengths is as follows:
10-week sessions Friday of the 7th week
8 – Week sessions Friday of the 6th week
5 – Week sessions Friday of the 3rd week
The equivalent date (75% of the semester) will be used for sessions of other
lengths. The specific last day to withdraw is published each semester in the
Schedule Bulletin.
PHYS 1403
4
Students who officially withdraw will be awarded the grade of “W” provided the
student’s attendance and academic performance are satisfactory at the time of
official withdrawal. Students must file a withdrawal application with the college
before they may be considered for withdrawal.
A student may not withdraw from a class for which the instructor has previously
issued the student a grade of “F” or “FN” for nonattendance.
B.
An Administrative Withdrawal: An administrative withdrawal may be initiated
when the student fails to meet College attendance requirements. The instructor
will assign the appropriate grade on the Administrative Withdrawal Form for
submission to the registrar.
The following specific rules apply to absences: Each instructor shall keep a record
of class attendance. An administrative withdrawal will be submitted when a
student’s absences exceed four (4) class meetings, and in the opinion of the
instructor, the student cannot satisfactorily complete the course. The final
decision rests solely with the instructor. The instructor will note administrative
withdrawals as the grade of “F Non-Attendance” on the roll and record book. As
a matter of policy, administrative excuses from classes are not provided for any
reason. Regardless of the nature of the absence, students are responsible for
completing all course work covered during any absence.
C.
D.
An Incomplete Grade: The College catalog states, “An incomplete grade may be
given in those cases where the student has completed the majority of the course
work, but because of personal illness, death in the immediate family, or military
orders, the student is unable to complete the requirements for a course...” Prior
approval from the instructor is required before the grade of “I” is recorded. A
student who merely fails to show for the final examination will receive a zero for
the final and an “F” for the course.
Disability Support Services provides services to students who have appropriate
documentation of a disability. Students requiring accommodations for class are
responsible for contacting the Office of Disability Support Services (DSS) located
on the central campus. This service is available to all students, regardless of
location. Review the website at www.ctcd.edu/disability-support for further
information. Reasonable accommodations will be given in accordance with the
federal and state laws through the DSS office.
E.
Students are required to be on class on time.
F.
For complete information consult the College Catalog!
PHYS 1403
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VIII. COURSE OUTLINE
A.
Unit One: Charting the Heavens: The Foundations of Astronomy, The
Copernican Revolution: The Birth of Modern Science, Radiation: Information
from the Cosmos, Spectroscopy: The Inner Working of Atoms, Telescopes: The
Tools of Astronomy.
1.
PHYS 1403
Unit Objectives: Upon successful completion of this unit, the student will
be able to:
a.
Describe how scientists combine observation, theory, and testing in
their study of the universe.
b.
Percieve the size of the universe.
c.
Explain the concept of the celestial sphere and how we use angular
measurement to locate objects in the sky.
d.
Describe how and why the sun and the stars appear to change their
positions from night to night and from month to month.
e.
Explain why Earth’s rotation axis shifts slowly with time, and say
how this affects Earth’s seasons.
f.
Tell how our clocks and calendars are linked to earth’s rotation and
orbit around the Sun.
g.
Show how the relative motions of Earth, the Sun, and the Moon
lead to eclipses.
h.
Explain the simple geometric reasoning that allows astronomers to
measure the distances and sizes of otherwise inaccessible objects.
i.
Describe how some ancient civilizations attempted to explain the
heavens in terms of Earth-Centered models of the universe.
j.
Explain how the observed motions of the planets led to our modern
view of a Sun-Centered solar system.
k.
Describe the major contributions of Galileo and Kepler to our
understanding of the solar system.
l.
State Kepler’s laws of planetary motion.
m.
Explain how astronomers have measured the true size of the solar
system.
n.
State Newton’s laws of motion and universal gravitation and
explain how they account for Kepler’s laws.
o.
See the connection between physics and astronomy; specially, the
Newton’s laws of gravity & motion, Kepler’s laws of orbital
motion and Einstein’s laws of relativity.
p.
Explain how the law of gravitation enables us to measure the
masses of astronomical bodies.
q.
Describe the basic properties of wave motion.
r.
Tell how electromagnetic radiation transfers energy and
information
through interstellar space.
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aa.
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cc.
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hh.
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kk.
PHYS 1403
Describe the major regions of the electromagnetic spectrum and
explain how earth’s atmosphere affects our ability to make
astronomical observations at different wavelengths.
Explain what is meant by the term “blackbody radiation” and
describe the basic properties of such radiation.
Tell how we can determine the temperature of an object by
observing the radiation it emits.
Show how the relative motion between a source of radiation and its
observer can change the perceived wavelength of the radiation, and
explain the importance of this phenomenon to astronomy.
Describe the characteristics of continuous, emission, and
absorption spectra and the conditions under which each is
produced.
Explain the relation between emission and absorption lines and
what we can learn from those lines.
Specify the basic components of the atom and describe our modern
conception of its structure.
Discuss the observations that led scientists to conclude that light
has particle as well as wave properties.
Explain how electron transitions within atoms produce unique
emission and absorption features in the spectra of those atoms.
Describe the general features of spectra produced by molecules.
List and explain the kinds of information that can be obtained by
analyzing the spectra of astronomical objects.
Explain the significance of the various forms of light and how they
are used in astronomy.
Sketch and describe the kinds of telescopes, explain their use, and
learn how to use them.
Explain the particular advantages of reflecting telescopes for
astronomical use, and specify why very large telescopes are needed
for most astronomical studies.
Explain the purposes of some of the detectors used in astronomical
telescopes.
Describe how Earth’s atmosphere affects astronomical
observations, and discuss some of the current efforts to improve
ground-based astronomy.
Discuss the advantages and disadvantages of radio astronomy
compared with optical observations.
Explain how interferometry can enhance the usefulness of
astronomical observations.
Explain why some astronomical observations are best done from
space, and discuss the advantages and limitations of space-based
astronomy.
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ll.
2.
Learning Activities:
a.
b.
c.
d.
e.
f.
3.
Read the related text material prior to the lecture.
Attend class lectures and take notes.
Learn about prisms and gratings by hands-on activities.
Watch demonstrations on how telescopes function and are used.
Observe planetarium demonstrations.
Enjoy selected audio-visual material as appropriate.
Unit Outline:
a.
PHYS 1403
Say why it is important to make astronomical observations in
different regions of the electromagnetic spectrum.
Chapter 1: Charting the Heavens: The Foundations of Astronomy
1-1. Our Place in Space
i.
Scale
ii.
SI and USCS system & Distances
iii.
Evolving Planets
iv.
Earth’s Structure
v.
Scientific Notation
vi.
Astronomical Unit (AU)
vii.
Light Travel & Distance
viii. Emptiness of Space
ix.
Light Year (LY)
x.
Star Clusters and Gas Clouds
xi.
Our Galaxy
xii.
Cluster of Galaxies
xiii. Superclusters, Filaments, & Voids
xiv. Angular measures
xv.
Degree, minutes, seconds.
1-2.
Scientific Theory and the Scientific Method
i.
Hypothesis, theory
ii.
Theoretical model
iii.
Scientific method:
iv.
Theory, prediction, observation.
v.
Testing a theory, experiment and proof.
1-3.
The “Obvious” View
i.
Constellations in the sky
ii.
Grouping of stars
iii.
Astrology
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iv.
v.
vi.
vii.
viii.
PHYS 1403
The Celestial Sphere
The celestial poles
The celestial equator
The celestial coordinates
Declination and right ascension.
1-4.
Earth’s Orbital Motion
i.
Day-to-Day Changes
ii.
Solar day
iii.
Diurnal motion
iv.
Sidereal day
v.
Seasonal Changes
vi.
The Zodiac
vii.
The summer solstice
viii. The winter solstice
ix.
The seasons
x.
equinoxes
xi.
Autumnal equinox
xii.
Vernal equinox
xiii. Tropical year
xiv. Long-Term Changes
xv.
Precession
xvi. Sidereal year.
1-5.
Astronomical Timekeeping
i.
Meridian
ii.
Variations in the solar day
iii.
Mean solar day
iv.
Time zones
v.
Standard time
vi.
Greenwich mean time
vii.
Universal time
viii. Tropical year
ix.
Leap year
x.
Julian calendar
xi.
Gregorian calendar
1-6.
The Motion of the Moon
i.
Lunar Phases
ii.
Sidereal month
iii.
Synodic month
iv.
Eclipses
v.
Partial lunar eclipse
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vi.
vii.
viii.
ix.
x.
xi.
xii.
xiii.
xiv.
xv.
1-7.
b.
PHYS 1403
Total lunar eclipses
Partial solar eclipses
Total solar eclipses
Umbra
Penumbra
Annular eclipses
Eclipse seasons
Eclipse geometry
Eclipse seasons
Eclipse tracks.
The Measurement of Distance
i.
Triangulation and Parallax
ii.
Baseline
iii.
Trigonometry
iv.
Geometric scaling
v.
Cosmic distance scale
vi.
Sizing Up Planet Earth
vii.
Parallax Geometry
viii. Measurement of Earth’s radius.
Chapter 2: The Copernican Revolution: The Birth of Modern
2-1.
The Ancient Astronomy
i.
Stonehenge
ii.
The Big Horn Medicine Wheel
iii.
The Caracol Temple
iv.
The Sun Dagger
2-2.
The Geocentric Universe
i.
Observations of the Planets
ii.
Prograde Motion
iii.
Retrograde Motion
iv.
Planetary motion
v.
Inferior planets
vi.
Superior Planets
vii.
Inferior conjunction
viii. Superior conjunction
ix.
A Theoretical Model
x.
Geocentric Universe
xi.
Epicycle
xii.
Deferent
Science
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xiii.
xiv.
PHYS 1403
Ptolemaic model
Evaluating the Geocentric Model.
2-3.
The Heliocentric Model of the Solar System
i.
Nicolaus Copernicus
ii.
The Copernican revolution
iii.
The Foundations of the Copernican Revolution.
2-4.
The Birth of Modern Astronomy
i.
Galileo’s Historic Observation
ii.
Galilean Moons
iii.
I0, Europa, Ganymede, Callisto
iv.
Dialogue Concerning the Two Chief World Systems
v.
The Ascendancy of the Copernican System.
2-5.
The Laws of Planetary Motion
i.
Brahe’s Complex Data
ii.
Brahe’s observatory, Uraniborg
iii.
Kepler’s laws of planetary motion
iv.
Shapes of planetary orbits
v.
Ellipse
vi.
Focus (plural: foci)
vii.
Semimajor axis
viii. Eccentricity
2-6.
The Dimensions of the Solar System
i.
Solar Transit
ii.
Astronomical unit
2-7.
Newton’s Laws
i.
Newtonian Mechanics
ii.
Newton’s First law of motion
iii.
Newton’s 2nd law of motion
iv.
Newton’s 3rd law of motion
v.
Newton’s law of Universal Gravitation.
2-8.
Newtonian Mechanics
i.
Planetary Motion
ii.
Solar Gravity
iii.
Kepler’s Laws Reconsidered
iv.
Center of Mass
v.
Weighing the Sun
vi.
Orbits of two bodies
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vii.
viii.
c.
Escape Speed
The Circle of Scientific Progress.
Chapter 3: Radiation: Information from the Cosmos
3-1.
Information from the Skies
i.
Electromagnetic radiation
ii.
Light and Radiation
iii.
Visible (spectrum) light
iv.
Radio, infrared, ultraviolet rays
v.
X-rays and Gamma Rays
vi.
Wave motion (velocity)
vii.
Wavelength, period, frequency and amplitude
viii. Amplitude
ix.
The components of visible light
x.
Visible spectrum
0
xi.
PHYS 1403
Nanometer(nm), Angstrom ( A )
3-2.
Waves in What?
i.
Matter waves
ii.
Sound wave
iii.
Light wave
iv.
Interaction between charged particles
v.
Electric Field
vi.
Magnetic field
vii.
Electromagnetic waves
viii. The wave theory of radiation
ix.
What is light? Wave or Matter?
3-3.
The Electromagnetic Spectrum
i.
The spectrum of radiation
ii.
AM, FM radio wave
ii.
Infrared, visible, ultraviolet, X-rays, Gamma rays
iii.
Atmospheric Opacity
iv.
The Wave nature of radiation
v.
Diffraction
vi.
Interference
vii.
Polarization
3-4.
Thermal Radiation
i.
Temperature and motion
ii.
Kelvin scale
iii.
Blackbody Spectrum
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iv.
v.
vi.
vii.
viii.
ix.
x.
3-5.
d.
PHYS 1403
Blackbody Curves, Ideal versus Reality
The Radiation Laws
The Wien’s Law
Stefan’s Law
Astronomical Applications
Astronomical Thermometer
The Sun at many wavelengths
The Doppler Effect
i.
Redshift
ii.
Blueshift
iii.
Radial velocities
iv.
Measuring velocities with the Doppler Effect
Chapter 4: Spectroscopy: The Inner Workings of Atoms
4-1. Spectral Lines
i.
Spectroscope
ii.
Emission Lines
iii.
Absorption lines
iv.
Solar spectrum
v.
Kirchhoff’s Laws
vi.
Identifying starlight
4-2.
Atoms and Radiation
i.
Atomic Structure
ii.
A Model of Atom
iii.
Different Kinds of Atoms
iv.
Electron Shells
v.
Ground State
vi.
Classical Atom
vii.
Quantum Atom
viii. Radiation as particles
ix.
Photon
x.
The Photoelectric Effect
4-3.
The Formation of Spectral Lines
i.
The Excitation of Atoms
ii.
The Formation of a Spectrum
iii.
The Hydrogen Spectrum
iv.
The Fluorescence
v.
Kirchhoff’s Laws Explained
vi.
More Complex Spectra
vii.
Emission Nebula
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e.
PHYS 1403
4-4.
Molecules
i.
Chemical Bonds
ii.
Rotation and Vibration of molecules
iii.
Electron Transitions
iv.
Hydrogen spectra
v.
The Shapes of Spectral Lines
4-5.
Spectral-Line Analysis
i.
A spectroscopic Thermometer
ii.
Measurement of Radial Velocity
iii.
Line Broadening
iv.
Line profile
v.
Doppler shift
vi.
Thermal Broadening
vii.
Rotational Broadening
viii. Information from Spectral Lines
ix.
The Message of Starlight.
Chapter: 5: Telescopes: The Tools of Astronomy
5-1.
Optical Telescopes
i.
Refracting and Reflecting Telescopes
ii.
Refracting Lens
iii.
Reflecting Mirrors
iv.
Comparing Refractors and Reflectors
v.
Image Formation
vi.
Spherical Aberration
vii.
Chromatic Aberration
viii. Types of Reflecting Telescopes
ix.
Newtonian Telescopes
x.
Cassegrain Telescopes
xi.
HST Detectors
5-2.
Telescope Size
i.
Light Gathering Power
ii.
Resolving Power
iii.
Collecting Area
iv.
The Resolving Powers of a Telescope
v.
Angular resolution
vi.
Sensitivity
5-3.
Images and Detectors
i.
Image Acquisition
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ii.
iii.
iv.
v.
vi.
vii.
viii.
PHYS 1403
Charged-Coupled Devices (CCDs)
Image Processing
Background noises
Wide-Angled Views
Photometry
Photometer
Spectroscopy
5-4.
High-Resolution Astronomy
i.
Atmospheric Blurring
ii.
Atmospheric Turbulence
iii.
Seeing
iv.
Seeing disk
v.
Light Pollution
vi.
Active Optics
vii.
Real-Time Control
viii. Adaptive Optics
5-5.
Radio Astronomy
i.
Radio Telescopes
ii.
Early Observations
iii.
Essentials of Radio Telescopes
iv.
Arecibo Observatory
v.
The value of Radio Astronomy
vi.
Haystack Observatory
5-6.
Interferometry
i.
Interferometer
ii.
A Radio Interferometer
iii.
VLA Interferometer
iv.
Interferometry at other Wavelengths
v.
Optical Interferometry
5-7.
Space-Based Astronomy
i.
Infrared Astronomy
ii.
Infrared Telescopes
iii.
Ultrviolet Astronomy
iv.
Ultraviolet telescopes
v.
High-Energy Astronomy
vi.
Einstein Observatory
vii.
Chandra Observatory
viii. X-Ray Observatory
ix.
Gamma-Ray Astronomy
15
5-8.
B.
Unit Two:
1.
The Sun, The Family of Stars, The Interstellar Medium, and the
Star formation.
Unit Objectives: Upon completion of this unit, the student will be able to:
a.
b.
c.
d.
e.
f.
g.
h.
i.
j.
k.
l.
m.
n.
o.
p.
PHYS 1403
Full-Spectrum Coverage
i.
Objects studied in Radio frequency
ii.
Objects studied in Infrared frequency
iii.
Objects studied in Visible frequency
iv.
Objects studied in Ultraviolet frequency
v.
Objects studied in X-Ray frequency
vi.
Objects studied in Gamma ray frequency
Describe the general and specific characteristics of the sun; its
source of energy, mechanism of energy transfer from its core to its
exterior and mass loss.
Summarize the overall properties and internal structure of the Sun.
Describe the concept of luminosity, and explain how it is
measured.
Explain how studies of the solar surface tell us about the Sun’s
interior.
List and describe the outer layers of the Sun.
Discuss the nature and variability of the Sun’s magnetic field.
Describe the various types of solar activity and their relation to
solar magnetism.
Outline the process by which energy is produced in the Sun’s
interior.
Explain how observations of the Sun’s core changed our
understanding of fundamental physics.
Explain how stellar distances are determined.
Discuss the motions of the stars through space and how those
motions are measured from Earth.
Distinguish between luminosity and apparent brightness, and
explain how stellar luminosity is determined.
Explain the usefulness of classifying stars according to their colors,
surface temperatures, and spectral characteristics.
Explain how physical laws are used to estimate stellar sizes.
Describe how a Hertzsprung – Russell diagram is constructed and
used to identify stellar properties.
Explain how knowledge of a star’s spectroscopic properties can
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Learning Activities:
a.
b.
c.
d.
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3.
lead to an estimate of its distance.
Explain how the masses of stars are measured and how mass is
related to other stellar properties.
Summarize the composition and physical properties of the
interstellar medium.
Describe the characteristics of emission nebulae, and explain their
significance in the life cycle of stars.
Discuss the properties of dark interstellar clouds.
Specify the radio techniques used to probe the nature of interstellar
matter.
Discuss the nature and significance of interstellar molecules.
Summarize the sequence of events leading to the formation of a
star like our Sun.
Explain how the formation of a star depends on its mass.
Describe some of the observational evidence supporting the
modern theory of star formation.
Explain the nature of interstellar shock waves, and discuss their
possible role in the formation of stars.
Explain why stars form in clusters, and distinguish between open
and globular star clusters.
Read the related text material prior to the lecture
Attend class lectures and take notes
Observe the sky using the unaided eye
Explore the sky using the telescope
Answer assigned questions to check on comprehension.
Participate in planetarium demonstrations.
Enjoy selected audio-visual material as appropriate.
Unit Outline:
a.
Chapter 16: The Sun: Our Parent Star
16-1. Physical Properties of the Sun
i.
Overall Properties
ii.
Differential Spin
iii.
Surface temperature
iv.
Heat Flow in the Sun
v.
The Photosphere
PHYS 1403
17
vi.
vii.
viii.
ix.
The Chromosphere
The Solar Corona
Helioseismology
Luminosity
16-2. Solar interior
i.
Mathematical models
ii.
Hydrostatic Equilibrium
iii.
Solar Oscillation
iv.
Solar interior
v.
Energy Transport
vi.
Solar Granulation
16-3. The Sun’s Atmosphere
i.
Solar Spectrum
ii.
The spectral lines
iii.
The Transition Zone and the Corona
iv.
The Solar Wind
16-4. Solar Magnetism
i.
Sunspots and Active Regions
ii.
The Sunspot Cycle
iii.
The Sun’s Magnetic Cycle
iv.
Magnetic Cycles on other Stars
v.
Prominences and Flares
vi.
Coronal Activity
vii.
The Solar Constant
viii. Maunder minimum
16-5. The Active Sun
i.
Active regions
ii.
Prominences
iii.
Flares
iv.
Coronal mass rejection
v.
The Sun in X-Rays
vi.
Coronal Holes
vii.
Mass ejection
viii. The changing Solar Corona
16-6. The Heart of the Sun
i.
Solar Energy Production
ii.
Nuclear Binding Energy
iii.
Weak force, Strong force
PHYS 1403
18
iv.
v.
vi.
vii.
viii.
ix.
viii.
ix.
Nuclear Fission
Hydrogen Fusion
Charged Particle Interactions
Coulomb Barrier
Proton-Proton Chain
Deuterium, Positron
Energy transport
Radiative and Convective zone
16-7. Observations of Solar Neutrinos
i.
The Solar Neutrino Problem
ii.
The Davis solar neutrino experiment
iii.
Neutrino Detectors
iv.
Neutrino Physics and Standard Model
v.
Neutrino Telescopes
b.
Chapter 17: The Stars: Giants, Dwarfs, and the Main Sequence
17-1. Measuring Distances to the Stars
i.
The Surveyor’s Method
ii.
The Astronomer’s Method
iii.
Stellar Parallax
iv.
Parsec
v.
Proper Motion
vi.
Our nearest neighbors
17-2. Luminosity and Apparent Brightness
i.
Brightness and Distance
ii.
Flux
iii.
Absolute Visual Magnitude
iv.
Calculating Absolute Visual Magnitude
v.
Magnitude-Distance Formula
vi.
Distance Modulus
vii.
Luminosity
viii. Luminosity
ix.
Absolute bolometric magnitude
17-3. Stellar Temperatures
i.
Luminosity, Radius, and Temperature
ii.
Reading The H-R Diagram
iii.
Giants, Super giants, and Dwarfs
iv.
Luminosity Classification
v.
Spectroscopic Parallax
vi.
Color and Blackbody Curve
PHYS 1403
19
vii.
viii.
Stellar Spectra
Spectral Classification
17-4. Stellar Sizes
i.
Direct and Indirect Measurements
ii.
Giants and Dwarfs
iii.
Red giants
iv.
Red Supergiants
v.
White dwarf
17-5. The Hertzsprung-Russell Diagram
i.
Luminosity versus temperature
ii.
Colors of Stars
iii.
The Main Sequence
iv.
Blue Giants
v.
Blue Supergiants
vi.
Red Dwarfs
17-6. Extending the Cosmic Distance Scale
i.
Spectroscopic Parallax explained
ii.
Stellar Luminosity Classes
17-7. Stellar Masses
i.
Binary Stars
ii.
Visual Binaries
iii.
Spectroscopic Binaries
iv.
Eclipsing Binaries
v.
Mass Determination
17-8. Mass and Other Stellar Properties
i.
Stellar Mass Distribution
ii.
Stellar Radii and Luminosities
c.
Chapter 18: The Interstellar Medium
18-1. Interstellar Matter
i.
Gas and Dust
ii.
Milky Way Mosaic
iii.
Dark Clouds
iv.
Extinction and Reddening
v.
Extinction and Reddening
vi.
Dust Grain
vii.
Overall Density
PHYS 1403
20
viii.
ix.
Compositi0n
Dust Shape
18-2. Emission Nebulae
i.
Observation of Emission Nebulae
ii.
Dust Lanes
iii.
Galactic Plane
iv.
M20-M8 Region
v.
Trifid Nebula
vi.
Nebular Structure
vii.
Nebular Spectra
viii. Emission Nebulae
ix.
Emission Nebulae Spectrum
x.
Forbidden Lines
xi.
Orion Nebula
18-3. Dark Dust Clouds
i.
Obscuration of Visible Light
ii.
Obscuration and Emission
iii.
Absorption Spectra
iv.
Horsehead Nebula
v.
Absorption by Interstellar Clouds
18-4. 21-Centimeter Radiation
i.
Electron Spin
ii.
Spin Quantization
iii.
Radio Emission
18-5. Interstellar Molecules
i.
Molecular Spectral Lines
ii.
Molecular Emission
iii.
Molecular Tracers
d.
Chapter 19: Star Formation
19-1. Star-Forming Regions
i.
Star Birth in Giant Molecular Clouds
ii.
Heating by Contraction
iii.
Protostars
iv.
Evidence of Star Formation
v.
Young Stars in the Universe
vi.
Extragalactic Star Formation
vii.
Gravity and Heat
PHYS 1403
21
viii.
Modeling Star Formation
19-2. The Formation of Stars Like the Sun
i.
Stage:1 An Interstellar Cloud
ii.
Cloud Fragmentation
iii.
Stage2: A collapsing Cloud Fragment
iv.
Stage3: Fragmentation Ceases
v.
Protostar Character
vi.
Stage4: A Protostar
vii.
Protostar on the H-R Diagram
viii. Stage5: Protostellar Evolution
ix.
Stage6: A Newborn Star
x.
Stage7: The Main Srquence at Last
19-3. Stars of Other Masses
i.
The Zero-Age Main Sequence (ZAMS)
ii.
Protostellar Evolutionary Tracks
iii.
Failed Stars
iv.
Brown Dwarfs
19-4. Observations of Cloud Fragments and Protostars
i.
Evidence of Cloud Contraction
ii.
Observation of Brown Dwarfs
iii.
Evidence of Cloud Fragments
iv.
Evidence of Protostars
v.
Protostellar Winds
19-5. Shock Waves and Star Formation
i.
Shock waves in space
ii.
Protostellar Outflow
iii.
Generations of Star Formation
iv.
A wave of star Formation
19-6. Star Clusters
i.
Clusters and Associations
ii.
Clusters and Nebulae
iii.
The Cluster Environment
iv.
Cluster Lifetimes
v.
Discovery of Eta Carinae
PHYS 1403
22
C.
Unit 3: Stellar Evolution, Stellar Explosions, Neutron Stars, and The Milky Way Galaxy
1.
Unit Objectives: Upon completion of this unit, the student will be able to:
a.
b.
c.
d.
e.
f.
g.
h.
i.
j.
k.
l.
m.
n.
o.
p.
q.
r.
s.
t.
PHYS 1403
Explain why stars evolve off the main sequence.
Outline the events that occur as a Sun-line star evolves from the
main sequence to the giant branch.
Explain how the Sun will eventually come to fuse helium in its
core, and describe what happens when that occurs.
Summarize the stages in the death of a typical low-mass star, and
describe the resulting remnant.
Contrast the evolutionary histories of high-mass and low-mass
stars.
Discuss the observations that help verify the theory of stellar
evolution.
Explain how the evolution of stars in binary systems may differ
from that of isolated stars.
Explain how white dwarf in binary-star systems can become
explosive.
Summarize the sequence of events leading to the violent death of a
massive star.
Describe the two types of supernovae, and explain how each is
produced.
Describe the observational evidence for the occurrence of
supernovae in our Galaxy.
Explain the origin of elements heavier than helium, and discuss the
significance of these elements for the study of stellar evolution.
Outline how the universe continually recycles matter through stars
and the interstellar medium.
Describe the properties of neutron stars, and explain how these
strange objects are formed.
Explain the nature and origin of pulsars, and account for their
characteristic radiation.
List and explain some of the observable properties of neutron-star
binary systems.
Discuss the basic characteristics of gamma-ray bursts and some
theoretical attempts to explain them.
Describe how black holes are formed, and discuss their effects on
matter and radiation in their vicinity.
Describe Einstein’s theories of relativity, and discuss how they
relate to neutron stars and black holes.
Relate the phenomena that occur near black holes to the warping of
space around them.
23
u.
v.
w.
x.
y.
z.
aa.
2.
Learning Activities:
a.
b.
c.
d.
e.
f.
3.
Discuss the difficulties in observing black holes, and explain some
of the ways in which the presence of a black hole might be
detected.
Describe the overall structure of the Milky Way Galaxy, how the
various regions differ from one another.
Explain the importance of variable stars in determining the size
and shape of our Galaxy.
Describe the orbital paths of stars in different regions of the
Galaxy, and explain how these motions are accounted for by our
understanding of how the Galaxy formed.
Discuss some possible explanations for the existence of the spiral
arms observed in our own and many other galaxies.
Explain what studies of Galactic rotation about the size and mass
of our Galaxy, and discuss the possible nature of dark matter.
Describe some of the phenomena observed at the center of the
Galaxy.
Read the related text material prior to the lecture
Attend the lecture on topics
Observe the sky with the unaided eye.
Observe the sky using the telescope
Try to answer assigned questions to check on comprehension.
Watch selected slides and films as appropriate.
Unit Outline:
a.
Chapter 20: Stellar Evolution: The Life and Death of a Star
20-1
Leaving the Main-Sequence
i.
Stars and the Scientific Method
ii.
Hydrostatic equilibrium
iii.
Structural Change
iv.
Core hydrogen burning
v.
Star’s stability
vi.
The Life of a Main-Sequence Star
vii.
The Life Expectancies of Stars
20-2. Evolution of a Sun-like Star
i.
Stage 8: The Subgiant Branch
ii.
Solar Composition Change
iii.
Hydrogen-shell-burning
PHYS 1403
24
iv.
v.
iv.
v.
vi.
vii.
viii.
ix.
x.
xi.
xii.
xiii.
xiv.
Subgiant
Stage 9: The Red-Giant Branch
Explain what is redgiant branch
The CNO Cycle
Red Giant on the H-R Diagram
Stage 10: Helium Fusion
Helium Flash
Electron Degeneracy Pressure
Horizontal Branch
Stage 11: Back to the Giant Branch
Helium-Shell Burning
Helium Giant Branch
Reascending the Red-Giant Branch
20-3. The Death of a Low-Mass Star
i.
The Fires Go Out
ii.
G-Type Star Evolution
iii.
Stage 12: A Planetary Nebula
iv.
Red-Giant Instability
v.
Ejected Envelope
vi.
Stage 13: A White Dwarf
vii.
White Dwarf on the H-R Diagram
viii. Sirius Binary System
ix.
Distant White Dwarf
x.
Stage 14: A Black Dwarf
xi.
Comparing Theory with Reality
xii.
Learning Astronomy from History
20-4. Evolution of Stars More Massive than the Sun
i.
Red Supergiants
ii.
High-Mass Evolutionary Tracks
iii.
Mass loss from Giant Stars
iv.
The End of the Road
20-5. Observing Stellar Evolution in Star Clusters
i.
The Evolving Cluster H-R Diagram
ii.
Newborn Cluster H-R Diagram
iii.
Young Cluster H-R Diagram
iv.
The Theory of Stellar Evolution
v.
Old Cluster H-R Diagram
20-6. Stellar Evolution in Binary Systems
i.
Classification of Binary Stars
PHYS 1403
25
ii.
iii.
iv.
v.
vi.
vii.
b.
Roche Lobes
Mass-Transfer Binaries
Contact Binary
Close Binary-Star System
Binary Evolution
Algol Evolution
Chapter 21: Stellar Explosions: Novae, Supernovae, and the
Formation of the Elements
21-1. Life after Death for White Dwarfs
i.
Novae
ii.
Close Binary system
iii.
Nova Explosion
iv.
The fate of the Sun, Nova?
v.
Nova matter Ejection
21-2. The end of a High-Massive Star
i.
Fusion of Heavy Elements
ii.
Collapse of The Iron Core
iii.
Supernova
iv.
Photo disintegration
v.
Core-collapse supernova
vi.
Nuclear Masses and Nuclei
vii.
Heavy-Element Fusion
21-3. Supernovae
i.
Supernova’s progenitor
ii.
Novae and Supernovae
iii.
Supernova Light Curves
iv.
Carbon-Detonation Supernovae
v.
Supernova 1987A
vi.
Supernova Remnants
vii.
Two Types of Supernova
viii. Crab Supernova Remnant
ix.
The Crab in Motion
x.
Vela Supernova Remnant
21-4. The Formation of the Elements
i.
Types of Matter
ii.
115 elements
iii.
116 and 117 elements discovered
iv.
Abundance of Matter
PHYS 1403
26
v.
vi.
vii.
viii.
ix.
x.
xi.
xii.
xiii.
xiv.
xv.
Stellar Nucleosynthesis
Hydrogen and Helium Burning
Proton Fusion
Carbon Burning and Helium Capture
Helium Fusion
Carbon Fusion
Iron Formation
Alpha Process
Making Elements Beyond Iron
Making the Heaviest Elements
Observational Evidence for Stellar Nucleosynthesis
21-5. The Cycle of Stellar Evolution
i.
Supernova Energy Emission
ii.
Spectra of Stars
c.
Chapter 14: Neutron Stars and Black Holes
22-1. Neutron Stars and Black Holes: Strange States of Matter
i.
Neutron Stars
ii.
Stellar Remnants
iii.
Neutron-Star Properties
iv.
Neutron degeneracy pressure
v.
Neutron star’s rotaton
vi.
Neutron star’s magnetic field
22-2. Pulsars
i.
Pulsar Radiation
ii.
The lighthouse model
iii.
Neutron Stars and Pulsars
iv.
Crab Pulsar
v.
Gamma-Ray Pulsars
vi.
Isolated Neutron Stars
vii.
Binary Neutron Stars
22-3. Neutron-Star Binaries
i.
X-Ray Sources
ii.
Microquasar
iii.
Millisecond Pulsars
iv.
Pulsar Planets
22-4. Gamma-Ray Bursts
i.
Distances and Luminosities
PHYS 1403
27
ii.
iii.
iv.
Compton Gamma-Ray Observatory
Cosmolgical Distances
What causes the Bursts?
22-5. Black Holes
i.
The Final Stage of Stellar Evolution
ii.
Escape speed
iii.
Black Hole Properties
iv.
The Event Horizon
22-6. Einstein’s Theories of Relativity
i.
Special Relativity
ii.
The Michelson-Morley Experiment
iii.
The new laws of Motion
iv.
General Relativity
v.
Curved Space and Black Holes
22-7. Space Travel Near Black Holes
i.
Tidal Forces
ii.
Approaching the Event Horizon
iii.
Gravitational Redshift
iv.
Deep Down Inside
v.
Singularity
vi.
Quantum Gravity
22-8. Observational Evidence for Black Holes
i.
Stellar Transits
ii.
Black Holes in Binary System
iii.
Black Holes in Galaxies
iv.
Supermassive Black Holes
v.
Intermediate-Mass Black Holes
vi.
Tests of General Relativity
vii.
Do Black Holes Exists?
viii. Gravity Waves: A New Window on the Universe
d.
Chapter 23: The Milky Way Galaxy: A Spiral in Space
23-1. Our Milky Way Galaxy
i.
The structure of our Galaxy
ii.
Galactic Disk
iii.
Galactic Bulge
iv.
Galactic Halo
v.
Galactic Plane
PHYS 1403
28
vi.
vii.
Andromeda Structure
Spiral Galaxies
23-2. Measuring the Milky Way
i.
Stellar Population
ii.
Spiral Nebulae and Globular Clusters
iii.
A New Yardstick
iv.
Pulsating Variable Stars
v.
The Cosmic Distance Scale
vi.
Period-Luminosity Relationship
vii.
The size and shape of our Galaxy
viii. The Shapley-Curtis Debate
23-3. Galactic Structure
i.
Stellar Populations in Our Galaxy
ii.
The Spatial Distribution of Stars
iii.
Stellar Populations
iv.
Orbital Motion
23-4. The Formation of the Milky Way
i.
Observation
ii.
Formation
iii.
Merger of several systems
23-5. Galactic Spiral Arms
i.
Radio Maps of the Milky Way
ii.
Spiral Structure
iii.
Survival of the Spiral Arms
iv.
Differential Galactic Rotation
v.
Spiral Density Waves
vi.
Origin of the Spiral Structure
23-6. The Mass of the Milky Way Galaxy
i.
Weighing the Galaxy
ii.
Galactic Rotation
iii.
Rotation Curve
iv.
Dark Matter
v.
Dark Halo
vi.
The Search for Stellar Dark Matter
vii.
Missing Red Dwarf
viii. Gravitational Lensing
PHYS 1403
29
23-7. The Galactic Center
i
Galactic center close-up
ii.
Galactic Activity
iii.
The Central Black Hole
D.
Unit Four: Galaxies, Galaxies and Dark Matter, Cosmology, The Early Universe,
and Life in the Universe
1.
Unit Objectives: Upon completion of this unit, the student will be able to:
a.
b.
c.
d.
e.
f.
g.
h.
i.
j.
k.
l.
m.
n.
o.
p.
q.
r.
s.
t.
PHYS 1403
Describe the basic properties of normal galaxies.
Discuss the distance-measurement techniques that enable
astronomers to map the universe beyond the Milky Way.
Describe how galaxies are observed to clump into clusters.
State Hubble’s law and explain how it is used to derive distances to
the most remote objects in the observable universe.
Specify the basic differences between active and normal galaxies.
Describe some important features of active galaxies.
Explain what drives the central engine thought to power all active
galaxies.
Describe some of the methods used to determine the masses of
distant galaxies.
Explain why astronomers think that most of the matter in the
universe is invisible.
Discuss some theories of how galaxies form and evolve.
Explain the role of black holes and active galaxies in current
theories of galactic evolution.
Summarize what is known about the large-scale distribution of
galaxies in the universe.
Describe some techniques used by astronomers to probe the
universe on very large scales.
State the cosmological principle, and explain its significance and
observational underpinnings.
Explain what observations of the dark night sky tell us about the
age of the universe.
Describe the Big Ban theory of the expanding universe.
Discuss the possible outcomes of the present cosmic expansion.
Describe the relationship between the density of the universe and
the overall geometry of space.
Say why astronomers think the expansion of the universe is
accelerating, and discuss the cause.
Explain what dark energy implies for the composition and age of
30
u.
v.
w.
x.
y.
z.
aa.
bb.
cc.
dd.
ee.
ff.
gg.
2.
Learning Activities:
a.
b.
c.
d.
e.
f.
3.
the universe.
Describe the cosmic microwave background and explain its
importance to the science of cosmology.
Describe the characteristics of the universe immediately after its
birth.
Explain how matter emerged from the primeval fireball.
Describe how radiation and matter evolved as the universe
expanded and cooled.
Explain how and when the simplest nuclei formed.
Discuss the consequences of the formation of the first atoms.
Summarize the horizon and flatness problems and describe how the
theory of cosmic inflation solves them.
Describe the formation of large-scale structure in the cosmos.
Explain how studies of the microwave background allow
astronomers to test and quantify their models of the universe.
Summarize the process of cosmic evolution as it is currently
understood.
Evaluate the chances of finding life elsewhere in the solar system.
Summarize the various probabilities used to estimate the number
of advanced civilizations that might exist in the Galaxy.
Discuss some of the techniques we might use to search for
extraterrestrials and to communicate with them.
Read the related text material prior to the lecture (see lecture
schedule)
Attend the lecture on topics
Observe the sky with the unaided eye.
Observe the sky using the telescope
Answer assigned questions to check on comprehension.
Watch the selected slides and films as appropriate.
Unit Outline
a.
Chapter 24: Galaxies: Building Blocks of the Universe
24-1. Hubble’s Galaxy Classification
i.
Hubble Classification Scheme
ii.
Spiral Galaxies
iii.
Barred Spirals Galaxies
iv.
Elliptical Galaxies
v.
Dwarf Elliptical Galaxies
PHYS 1403
31
vi.
vii.
viii.
ix.
x.
Irregular Galaxies
Magellanic Clouds
Irregular Galaxy Shapes
The Hubble Sequence
The Galactic “Tuning Fork”
24-2. The Distribution of Galaxies in Space
i.
Extending the Distance Scale
ii.
Standard Candles
iii.
Tully-Fisher Relation
iv.
Cluster of Galaxies
v.
Local Group
24-3. Hubble’s Law
i.
Universal Recession
ii.
Hubble’s Constant
iii.
The top of the Distance Ladder
24-4. Active Galactic Nuclei
i.
Normal Galaxies
ii.
Galactic Radiation
iii.
Galaxy Energy Spectra
iv.
Active Galaxy
v.
Seyfert Galaxies
vi.
Relativistic Redshifts and Look-Back Time
vii.
Radio Galaxies
viii. Radio Lobes
ix.
Quasars
24-5. The Central Engine of an Active Galaxy
i.
Energy Production
ii.
Active Galactic Nucleus
iii.
Energy Emission
iv.
Dusty Donut
v.
Nonthermal Radiation
vi.
Synchrotron Radiation
b.
Chapter 25: Galaxies and Dark Matter: The Large-Scale Structure
of the Cosmos
25-1. Dark Matter in the Universe
i.
Masses of Galaxies and Galaxy Clusters
ii.
Galaxy Rotation Curves
PHYS 1403
32
iii.
iv.
v.
vi.
Galaxy Masses
Visible Matter and Dark Halos
Dark Galaxy
Intracluster Gas
25-2. Galaxy Collisions
i.
Cosmic Cartwheel
ii.
Galaxy Encounter
iii.
Collision is common phenomena
iv.
Merger
v.
Milky Way Collision
25-3. Galaxy Formation and Evolution
i.
Mergers and Acquisition
ii.
Hierarchical Merging
iii.
Evolution and Interaction
iv.
Starburst Galaxies
v.
Types of Merger
vi.
Making the Hubble Sequence
vii.
Tidal Streams in the Milky Way
25-4. Black Holes in Galaxies
i.
Black Hole Masses
ii.
The Quasar Epoch
iii.
Active and Normal Galaxies
iv.
Active Galaxies and the Scientific Method
25-5. The Universe on Large Scales
i.
Clusters of Clusters
ii.
Galaxy Evolution
iii.
Superclusters
iv.
Redshift Survey
v.
Local Supercluster
vi.
Virgo Supercluster in 3-D
vii.
Galaxy Survey
viii. Quasar Absorption Lines
ix.
The Universe on Larger Scales
x.
The Sloan Digital Sky Survey
xi.
Quasar “Mirages”
xii.
Gravitational Lens
xiii. Mapping Dark Matter
PHYS 1403
33
c.
Chapter 26: Cosmology: The Big Bang and the Fate of the
Universe
26-1. The Universe on the Largest Scales
i.
Cosmology
ii.
The End of Structur
iii.
Galaxy Survey
iv.
The Cosmological Principle
v.
Isotropic
vi.
Pencil-Beam Survey
vii.
A stunning View of Deep Space
26-2. The Expanding Universe
i.
Olbers’s Paradox
ii.
The Birth of the Universe
iii.
Primeval Fireball
iv.
Where was the Big Bang?
v.
The Cosmological Redshift
26-3. The Fate of the Cosmos
i.
Critical Density
ii.
Escape Speed
iii.
Critical Density
iv.
Model Universe
v.
Two Futures of our Universe
26-4. The Geometry of Space
i.
Relativity and the Universe
ii.
Cosmic Curvature
iii.
Curved Space
iv.
Closed Universe
v.
Open Universe
26-5. Will the Universe Expand Forever?
i.
The Density of the Universe
ii.
Cosmic Acceleration
iii.
Dark Energy
iv.
Cosmological Constant
v.
Quintessence
26-6. Dark Energy and Cosmology
i.
The Composition of the Universe
PHYS 1403
34
ii.
iii.
Geometry of the Universe
Cosmic Age Estimates
26-7: The Cosmic Microwave Background
i.
Discovery
ii.
2.7 K Temperature
iii.
Cosmic Blackbody Curves
iv.
Microwave Background Spectrum
v.
Microwave Sky
d.
Chapter 27: The Early Universe: Toward the Beginning of Time
27-1. Back to the Big Bang
i.
Cosmic Composition
ii.
Radiation in the Universe
iii.
Radiation-Matter Dominance
iv.
Particle production
v.
Pair Production
vi.
Thermal Equilibrium
27-2. The Evolution of the Universe
i.
Before the Big Bang?
ii.
The Radiation Era
iii.
Grand Unified Theories
iv.
Freeze-Out
v.
Quarks and Leptons
vi.
More on Fundamental Forces
vii.
The Matter and Dark-Energy Eras
27-3. The Formation of Nuclei and Atoms
i.
Helium Formation in the Early Universe
ii.
Deuterium and the Density of the Cosmos
iii.
The First Atoms
iv.
Radiation-Matter Decoupling
27-4. The Inflationary Universe
i.
The Horizon and Flatness Problems
ii.
Cosmic Inflation
iii.
Scalar Fields
iv.
Vacuum Energy
v.
Epoch of Inflation
vi.
Implications for the Universe
vii.
Inflation as a Theory
PHYS 1403
35
27-5. The Formation of Structure in the Universe
i.
The Growth of Inhomogeneities
ii.
Dark Matter
iii.
Hot dark Matter
iv.
Cold Dark Matter
27-6. Cosmic Structure and the Microwave Background
i.
Cosmic Microwave Background Map
ii.
Early Structure
e.
PHYS 1403
Chapter 28: Life in the Universe: Are We Alone?
28-1
Cosmic Evolution
i.
Life in the Universe
ii.
Arrow of Time
iii.
Chemical Evolution
iv.
Amino acids and nucleotide
v.
Urey-Miller Experiment
vi.
An Interstellar Origin
vii.
Diversity and Culture
28-2
Life in the Solar System
i.
Life as we Know it
ii.
Search for Martian Life
iii.
Extremophiles
iv.
Alternative Biochemistries
28-3
Intelligent Life in the Galaxy
i.
The Drake Equation
ii.
Rate of Star Formation
iii.
Fraction of Stars Having Planetary System
iv.
Number of Habitable Planets per Planetary System
v.
Fraction of Habitable Planets on Which Life
Actually Arises
vi.
Fraction of Life-Bearing Planets on Which
Intelligence Arises
vii.
Fraction of Planets on Which Intelligent Life
Develops and Uses Technology
viii. Average Lifetime of a Technological Civilization
ix.
Number of Technological Civilizations in the
Galaxy
36
28-4. The Search for Extraterrestrial Intelligence
i. Meeting Our Neighbors
ii. Pioneer 10 Plaque
iii. Radio Communication
iv. The Water Hole
v. Leakage
vi. Project Phoenix
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37