Discover the beauty and simplicity of science's most fundamental branch with Physics and Our Universe: How It All Works. Intensively illustrated with diagrams, experiments, animations, graphs, and other visual aids, these 60 lectures by engaging and award-winning Professor Richard Wolfson introduce you to scores of fundamental ideas such as Newtonian mechanics, waves and fluids, thermodynamics, electricity and magnetism, optics, and relativity and quantum theory.
Physics and Our Universe
An award-winning professor brings physics down to earth from everyday examples to universal principles.
Rated 4 out of
5
by
london2000 from
A good course, but long and intense
Sixty lectures long, this is undoubtedly the broadest and deepest course I have completed on this platform. Richard Wolfson knows his physics backwards, and speaks rapidly and fluently - no one could accuse him of reading a script from an autocue! His enthusiasm is infectious and his practical demonstrations of some key features of physics were very effective to watch.
Nonetheless, the course felt like a whirlwind tour of physics and despite me having a scientific background, with a familiarity of much of his material, albeit from many years ago, I felt it was often too rushed. This was particularly so when Richard was going through calculations on the big monitor. I feel that a course of this breadth and magnitude needed more than sixty lectures, which is not feasible. Therefore, it may have been better to have split it into two or more courses, each covering different aspects of physics.
Date published: 2024-11-04
Rated 5 out of
5
by
Gharmjo from
Best Value for Money in TGC catalog
Wolfson comprehensively reviews physics and illustrates it via brilliant experiments. The course uses basic algebra but it is also safe to just trust his “anatomy of equations” (see Lecture 28=L28). But the math opens up a depth of knowledge unavailable before (see L47-48 comments below). His speech is rapid, often providing multiple viewpoints of a concept within a single “paragraph". The scope is massive, omitting only complexity theory (see the Great Course "Chaos" by Strogatz). NO REVIEW CAN DO JUSTICE to this course and Wolfson’s output greatly exceeds the 382-page Guidebook. Take notes, buy the course transcript, or (best) redo the course several times.
RANDOM WALKS: L4: If in the same orbit as the space station, one can’t just accelerate to get there. Nope…have to decelerate to lower orbit, coast to near the station using the lower orbit's shorter path, and then precisely fire rockets to ascend to the station. L16 discusses a “metastable" state where things are neither fully stable nor unstable. [Wolfson’s Great Course “Understanding Modern Electronics" discusses electronic component metastable states] L16 then says that in two+ dimensions, metastable states become “more complex”. Indeed! A neighbor’s auto transmission electronics at unpredictable intervals disagrees with its electronic control panel...and the car in "Drive" remains parked with a "P" reading on the dash! L17: Due to the parabolic shape of most potential energy stable-equilibrium curves: “any systems in the universe that are 'stable’…undergo harmonic motion…(which is therefore) ubiquitous throughout the universe.” Ex: atmospheric CO2’s different harmonic oscillations absorb multiple I.R. doses.
L23: “Emissivity (the amount of radiation heat) of a thermos bottle is close to zero because the bottle is shiny” while its vacuum prevents conductional convection. L24’s formula PV = NKT (N is # molecules, K Boltzman's constant, n is the # moles and R is the gas constant) for an ideal gas (when molecules are far apart) seemed “wrong". Wolfson paused and then explained why we chemistry majors know this as PV = nRT. L25's experiment shows adiabatic (no external heat flow vs. isothermal with a constant temp) compression igniting a tissue paper by massive air compression, explaining diesel engines. This immediately led to Chinook winds where cool air coming down mountains heats adiabatically making them warm when they reach the plains. L28: Wolfson's marvelous humility: “What is electric charge? Well, it beats me" and “I really don't know what mass is" - admit a few of the limits of the “religion of science".
L30 is astounding in its rigor: from battery physics to electron dipole equipotential mapping to cardiac mapping (EKGs are a subset). Ex: Any sharp corner/fastener in a power line can create concentrated electrical fields strong enough to cause air breakdown and sparking. L30-38: add enormous depth to his Electronics course. L47-48’s time dilation equations for correcting time in relativity are EASIER to comprehend than a rote acceptance of relativity’s consequences. L50: Max Plank's forced solution to the "UV catastrophe” led to his equation for light bulb variability. It soon became recognized as a solution for any quantized vibrational oscillatory atomic/molecular glowing process...opening up quantum physics. L51 provides a brilliant lab where a closed wire loop subjected to increasing frequencies suddenly jumps into an integer multiple of wavelengths with a node-like structure…illustrating Bohr's math approach to quantized orbital theory. L53: Computerization of the Schrodinger equation allows prediction of molecular function. Though electrons at equilibrium occupy quantized positions within quantum harmonic oscillators, there is a nonzero probability of finding a particle where classical energy conservation prohibits it. This provides life (via permitting solar fusion), radioactive decay, and even tunneling microscopes. The last 6L range from chemistry to dark energy.
WOLFSON’S WARNING: Wolfson warns in L48 (and his Great Course “Einstein's Relativity", L12) that Relativity can ONLY be applied to “an objective physical reality”. He laments that the Humanities have WRONGLY decided: “If everything is relative, then all is relative in our field too”. Could recognizing this gross Humanities error end today’s "elitist" self-contradictions?
Date published: 2024-03-11
Rated 5 out of
5
by
cpr_norcal from
Top Notch in Every Respect
As Many have noted, Prof. Wolfson's enthusiasm and energy is compelling, and his lectures are wonderfully crafted. He The graphical illustrations and the experiments were put together in such illustrative ways. The math was a little daunting at times however the logic behind it is explained so well that one need not digest every smallest detail.
I've viewed well over a hundred courses from TGC/Wondrium and this is at the topmost tier for me.
Date published: 2023-12-19
Rated 5 out of
5
by
syed49 from
Great conceptual overview of latest Physics
Dr. Wolfson presents an overview of all of Physics in a most engaging and interesting style. He has the capability to present extremely difficult concepts in a way that can be understood by even non-experts. I found this course to be very stimulating and it fulfilled my long time desire to understand more about our universe. I fill followup some of the concepts outlined by Dr. Wolfson by additional readings. Thanks for a wonderful course
Date published: 2023-05-01
Rated 5 out of
5
by
kidbill449 from
physics and our universe
love this course bought Dr.W text book as a result wish I could get the solutions set
for self study minor error on rotational instead of alpha being change in omega/time
says change in theta/time which would be angular velocity
Date published: 2023-01-10
Rated 5 out of
5
by
Stormy97 from
Great Survey of Pretty Much All of Physics!!
This is a great survey of pretty much all of physics. The prof is very engaging and enthusiastic about the subject. I've noticed criticism that he runs through the algebra very quickly which is true, but it just requires some effort to keep up. My only criticism is that, perhaps by necessity, he oversimplified the section on electromagnetism. I still would like to understand how electric power is transmitted and the course does really not explain that but it does provide the background for exploring the subject at a deeper level.
Date published: 2022-11-25
Rated 5 out of
5
by
elshrimp from
Met expectations and beyond
It was well taught, understandable, covered the material I was looking for and beyond. I came out very satisfied and now I understand much more than before. You come out with a good feeling.
Date published: 2022-10-29
Rated 5 out of
5
by
odolha from
Wish it was longer
Don't get me wrong. This was a marathon.
But still, I think it was rushed a bit because of the vast amount of material to cover.
I think the professor did an impeccable job of organizing and presenting basically most of all physics, suitable to most people, with vast backgrounds. I think pretty much anyone could follow this course, even if some courses may require repetition or rewinding at times.
Personally, I wish the professor would have a more advanced course paralleling this one, where he could dive deeper (should probably be even longer), and with more advanced mathematics. But even so I enjoyed this course tremendously and can't wait to watch some other of his courses.
Many thanks!
Date published: 2022-10-25
Overview
About
Dr. Richard Wolfson is the Benjamin F. Wissler Professor of Physics at Middlebury College, where he also teaches Climate Change in Middlebury's Environmental Studies Program. He completed his undergraduate work at MIT and Swarthmore College, graduating from Swarthmore with a double major in Physics and Philosophy. He holds a master's degree in Environmental Studies from the University of Michigan and a Ph.D. in Physics from Dartmouth.
Professor Wolfson's published work encompasses diverse fields such as medical physics, plasma physics, solar energy engineering, electronic circuit design, observational astronomy, theoretical astrophysics, nuclear issues, and climate change. His current research involves the eruptive behavior of the sun's outer atmosphere, or corona, as well as terrestrial climate change and the sun-Earth connection.
Professor Wolfson is the author of several books, including the college textbooks Physics for Scientists and Engineers, Essential University Physics,and Energy, Environment, and Climate. He is also an interpreter of science for the nonspecialist, a contributor to Scientific American, and author of the books Nuclear Choices: A Citizen's Guide to Nuclear Technology and Simply Einstein: Relativity Demystified.
Trailer
01: The Fundamental Science
Take a quick trip from the subatomic to the galactic realm as an introduction to physics, the science that explains physical reality at all scales. Professor Wolfson shows how physics is the fundamental science that underlies all the natural sciences. He also describes phenomena that are still beyond its explanatory power.
31 min
02: Languages of Physics
Understanding physics is as much about language as it is about mathematics. Begin by looking at how ordinary terms, such as theory and uncertainty, have a precise meaning in physics. Learn how fundamental units are defined. Then get a taste of the basic algebra that is used throughout the course.
31 min
03: Describing Motion
Motion is everywhere, at all scales. Learn the difference between distance and displacement, and between speed and velocity. Add to these the concept of acceleration, which is the rate of change of velocity, and you are ready to delve deeper into the fundamentals of motion.
28 min
04: Falling Freely
Use concepts from the previous lecture to analyze motion when an object is under constant acceleration due to gravity. In principle, the initial conditions in such cases allow the position of the object to be determined for any time in the future, which is the idea behind Isaac Newton's "clockwork universe."
30 min
05: It's a 3-D World!
Add the concept of vector to your physics toolbox. Vectors allow you to specify the magnitude and direction of a quantity such as velocity. The vector's direction can be along any axis, allowing analysis of motion in three dimensions. Then use vectors to solve several problems in projectile motion.
29 min
06: Going in Circles
Circular motion is accelerated motion, even if the speed is constant, because the direction, and hence the velocity, is changing. Analyze cases of uniform and non-uniform circular motion. Then close with a problem challenging you to pull out of a dive in a jet plane without blacking out or crashing.
30 min
07: Causes of Motion
For most people, the hardest part of learning physics is to stop thinking like Aristotle, who believed that force causes motion. It doesn't. Force causes change in motion. Learn how Galileo's realization of this principle, and Newton's later formulation of his three laws of motion, launched classical physics.
30 min
08: Using Newton's Laws-1-D motion
Investigate Newton's second law, which relates force, mass, and acceleration. Focus on gravity, which results in a force, called weight, that's proportional to an object's mass. Then take a ride in an elevator to see how your measured weight changes due to acceleration during ascent and descent.
32 min
09: Action and Reaction
According to Newton's third law, "for every action there is an equal and opposite reaction." Professor Wolfson has a clearer way of expressing this much-misunderstood phrase. Also, see several demonstrations of action and reaction, and learn about frictional forces through examples such as antilock brakes.
30 min
10: Newton's Laws in 2 and 3 Dimensions
Consider Newton's laws in cases of two and three dimensions. For example, how fast does a rollercoaster have to travel at the top of a loop to keep passengers from falling out? Is there a force pushing passengers up as the coaster reaches the top of its arc? The answer may surprise you.
30 min
11: Work and Energy
See how the precise definition of work leads to the concept of energy. Then explore how some forces "give back" the work done against them. These conservative forces lead to the concept of stored potential energy, which can be converted to kinetic energy. From here, develop the important idea of conservation of energy.
31 min
12: Using Energy Conservation
A dramatic demonstration with a bowling ball pendulum shows how conservation of energy is a principle you can depend on. Next, solve problems in complicated motion using conservation of energy as a shortcut. Close by drawing the distinction between energy and power, which are often confused.
30 min
13: Gravity
Newton realized that the same force that makes an apple fall to the ground also keeps the moon in its orbit around Earth. Explore this force, called gravity, by focusing on circular orbits. End by analyzing why an orbiting spacecraft has to decrease its kinetic energy in order to speed up.
30 min
14: Systems of Particles
How do you analyze a complex system in motion? One special point in the system, called the center of mass, reduces the problem to its simplest form. Also learn how a system's momentum is unchanged unless external forces act on it. Then apply the conservation of momentum principle to analyze inelastic and elastic collisions.
30 min
15: Rotational Motion
Turn your attention to rotational motion. Rotational analogs of acceleration, force, and mass obey a law related to Newton's second law. This leads to the concept of angular momentum and the all-important -conservation of angular momentum, which explains some surprising and seemingly counterintuitive phenomena involving rotating objects.
33 min
16: Keeping Still
What's the safest angle to lean a ladder against a wall to keep the ladder from slipping and falling? This is a problem in static equilibrium, which is the state in which no net force or torque (rotational force) is acting. Explore this condition and develop tools for determining whether equilibrium is stable or unstable.
30 min
17: Back and Forth-Oscillatory Motion
Start a new section in which you apply Newtonian mechanics to more complex motions. In this lecture, study oscillations, a universal phenomenon in systems displaced from equilibrium. A special case is simple harmonic motion, exhibited by springs, pendulums, and even molecules.
32 min
18: Making Waves
Investigate waves, which transport energy but not matter. When two waves coexist at the same point, they interfere, resulting in useful and surprising applications. Also examine the Doppler effect, and see what happens when an object moves through a medium faster than the wave speed in that medium.
28 min
19: Fluid Statics-The Tip of the Iceberg
Fluid is matter in a liquid or gaseous state. In this lecture, study the characteristics of fluids at rest. Learn why water pressure increases with depth, and air pressure decreases with height. Greater pressure with depth causes buoyancy, which applies to balloons as well as boats and icebergs.
30 min
20: Fluid Dynamics
Explore fluids in motion. Energy conservation requires low pressure where fluid velocity is high, and vice versa. This relation between pressure and velocity results in many practical and sometimes counterintuitive phenomena, collectively called the Bernoulli effect-explaining why baseballs curve and how airplane speedometers work.
31 min
21: Heat and Temperature
Beginning a new section, learn that heat is a flow of energy driven by a temperature difference. Temperature can be measured with various techniques but is most usefully quantified on the Kelvin scale. Investigate heat capacity and specific heat, and solve problems in heating a house and cooling a nuclear reactor.
29 min
22: Heat Transfer
Analyze heat flow, which involves three important heat-transfer mechanisms: conduction, which results from direct molecular contact; convection, involving the bulk motion of a fluid; and radiation, which transfers energy by electromagnetic waves. Study examples of heat flow in buildings and in the sun's interior.
31 min
23: Matter and Heat
Heat flow into a substance usually raises its temperature. But it can have other effects, including thermal expansion and changes between solid, liquid, and gaseous forms-collectively called phase changes. Investigate these phenomena, starting with an experiment in which Professor Wolfson pours liquid nitrogen onto a balloon filled with air.
30 min
24: The Ideal Gas
Delve into the deep link between thermodynamics, which looks at heat on the macroscopic scale, and statistical mechanics, which views it on the molecular level. Your starting point is the ideal gas law, which approximates the behavior of many gases, showing how temperature, pressure, and volume are connected by a simple formula.
31 min
25: Heat and Work
The first law of thermodynamics relates the internal energy of a system to the exchange of heat and mechanical work. Focus on isothermal (constant temperature) and adiabatic (no heat flow) processes, and see how they apply to diesel engines and the atmosphere.
31 min
26: Entropy-The Second Law of Thermodynamics
Turn to an idea that has been compared to a work of Shakespeare: the second law of thermodynamics. According to the second law, entropy, a measure of disorder, always increases in a closed system. Order can only increase at the cost of even greater entropy elsewhere in the system.
31 min
27: Consequences of the Second Law
The second law puts limits on the efficiency of heat engines and shows that humankind's energy use could be better planned. Learn why it makes sense to exploit low-entropy, high-quality energy for uses such as transportation, motors, and electronics, while using high-entropy random thermal energy for heating.
31 min
28: A Charged World
Embark on a new section of the course, devoted to electromagnetism. Begin by investigating electric charge, which is a fundamental property of matter. Coulomb's law states that the electric force depends on the product of the charges and inversely on the square of the distance between them.
32 min
29: The Electric Field
On of the most important ideas in physics is the field, which maps the presence and magnitude of a force at different points in space. Explore the concept of the electric field, and learn how Gauss's law describes the field lines emerging from an enclosed charge.
31 min
30: Electric Potential
Jolt your understanding of electric potential difference, or voltage. A volt is one joule of work or energy per coulomb of charge. Survey the characteristics of voltage-from batteries, to Van de Graaff generators, to thunderstorms, which discharge lightning across a potential difference of millions of volts.
31 min
31: Electric Energy
Study stored electric potential energy in fuels such as gasoline, where the molecular bonds represent an enormous amount of energy ready to be released. Also look at a ubiquitous electronic component called the capacitor, which stores an electric charge, and discover that all electric fields represent stored energy.
29 min
32: Electric Current
Learn the definition of the unit of electric current, called the ampere, and how Ohm's law relates the current in common conductors to the voltage across the conductor and the conductor's resistance. Apply Ohm's law to a hard-starting car, and survey tips for handling electricity safely.
30 min
33: Electric Circuits
All electric circuits need an energy source, such as a battery. Learn what happens inside a battery, and analyze simple circuits in series and in parallel, involving one or more resistors. When capacitors are incorporated into circuits, they store electric energy and introduce time dependence into the circuit's behavior.
31 min
34: Magnetism
In this introduction to magnetism, discover that magnetic phenomena are really about electricity, since magnetism involves moving electric charge. Learn the right-hand rule for the direction of magnetic force. Also investigate how a current-carrying wire in a magnetic field is the principle behind electric motors.
29 min
35: The Origin of Magnetism
No matter how many times you break a magnet apart, each piece has a north and south pole. Why? Search for the origin of magnetism and learn how magnetic field lines differ from those of an electric field, and why Earth has a magnetic field.
30 min
36: Electromagnetic Induction
Probe one of the most fascinating phenomena in all of physics, electromagnetic induction, which shows the direct relationship between electric and magnetic fields. In a demonstration with moving magnets, see how the relative motion of a magnet and an electric conductor induces current in the conductor.
31 min
37: Applications of Electromagnetic Induction
Survey some of the technologies that exploit electromagnetic induction: the electric generators that supply nearly all the world's electrical energy, transformers that step voltage up or down for different uses, airport metal detectors, microphones, electric guitars, and induction stovetops, among many other applications.
29 min
38: Magnetic Energy
Study the phenomenon of self-inductance in a solenoid coil, finding that the magnetic field within the coil is a repository of magnetic energy, analogous to the electric energy stored in a capacitor. Close by comparing the complementary aspects of electricity and magnetism.
30 min
39: AC/DC
Direct current (DC) is electric current that flows in one direction; alternating current (AC) flows back and forth. Learn how capacitors and inductors respond to AC by alternately storing and releasing energy. Combining a capacitor and inductor in a circuit provides the electrical analog of simple harmonic motion introduced in Lecture 17.
31 min
40: Electromagnetic Waves
Explore the remarkable insight of physicist James Clerk Maxwell in the 1860s that changing electric fields give rise to magnetic fields in the same way that changing magnetic fields produce electric fields. Together, these changing fields result in electromagnetic waves, one component of which is visible light.
30 min
41: Reflection and Refraction
Starting a new section of the course, discover that light often behaves as rays, which change direction at boundaries between materials. Investigate reflection and refraction, answering such questions as, why doesn't a dust mote block data on a CD? How do mirrors work? And why do diamonds sparkle?
31 min
42: Imaging
See how curving a mirror or a piece of glass bends parallel light rays to a focal point, allowing formation of images. Learn how images can be enlarged or reduced, and the difference between virtual and real images. Use your knowledge of optics to solve problems in vision correction.
30 min
43: Wave Optics
Returning to themes from Lecture 18 on waves, discover that when light interacts with objects comparable in size to its wavelength, then its wave nature becomes obvious. Examine interference and diffraction, and see how these effects open the door to certain investigations, while hindering others.
33 min
44: Cracks in the Classical Picture
Embark on the final section of the course, which covers the revolutionary theories that superseded classical physics. Why did classical physics need to be replaced? Discover that by the late 19th century, inexplicable cracks were beginning to appear in its explanatory power.
30 min
45: Earth, Ether, Light
Review the famous Michelson-Morley experiment, which was designed to detect the motion of Earth relative to a conjectured "ether wind" that supposedly pervaded all of space. The failure to detect any such motion revealed a deep-seated contradiction at the heart of physics.
31 min
46: Special Relativity
Discover the startling consequences of Einstein's principle of relativity-that the laws of physics are the same for all observers in uniform motion. One result is that the speed of light is the same for all observers, no matter what their relative motion-an idea that overturns the concept of simultaneity.
30 min
47: Time and Space
Einstein's special theory of relativity upends traditional notions of space and time. Solve the simple formulas that show the reality of time dilation and length contraction. Conclude by examining the twins paradox, discovering why one twin who travels to a star and then returns ages more slowly than the twin back on Earth.
31 min
48: Space-Time and Mass-Energy
In relativity theory, contrary to popular views, reality is what's not relative-that is, what doesn't depend on one's frame of reference. See how space and time constitute one such pair, merging into a four-dimensional space-time. Mass and energy similarly join, related by Einstein's famous E = mc2.
31 min
49: General Relativity
Special relativity is limited to reference frames in uniform motion. Following Einstein, make the leap to a more general theory that encompasses accelerated frames of reference and necessarily includes gravity. According to Einstein's general theory of relativity, gravity is not a force but the geometrical structure of spacetime.
30 min
50: Introducing the Quantum
Begin your study of the ideas that revolutionized physics at the atomic scale: quantum theory. The word "quantum" comes from Max Planck's proposal in 1900 that the atomic vibrations that produce light must be quantized-that is, they occur only with certain discrete energies.
30 min
51: Atomic Quandaries
Apply what you've learned so far to work out the details of Niels Bohr's model of the atom, which patches one of the cracks in classical physics from Lecture 44. Although it explains the energies of photons emitted by simple atoms, Bohr's model has serious limitations.
31 min
52: Wave or Particle?
In the 1920s physicists established that light and matter display both wave- and particle-like behavior. Probe the nature of this apparent contradiction and the meaning of Werner Heisenberg's famous uncertainty principle, which introduces a fundamental indeterminacy into physics.
31 min
53: Quantum Mechanics
In 1926 Erwin Schrödinger developed an equation that underlies much of our modern quantum-mechanical description of physical reality. Solve a simple problem with the Schrödinger equation. Then learn how the merger of quantum mechanics and special relativity led to the discovery of antimatter.
32 min
54: Atoms
Drawing on what you now know about quantum mechanics, analyze how atoms work, discovering that the electron is not a point particle but behaves like a probability cloud. Investigate the exclusion principle, and learn how quantum mechanics explains the periodic table of elements and the principle behind lasers.
31 min
55: Molecules and Solids
See how atoms join to make molecules and solids, and how this leads to the quantum effects that underlie semiconductor electronics. Also probe the behavior of matter in ultradense white dwarfs and neutron stars, and learn how a quantum-mechanical pairing of electrons at low temperatures produces superconductivity.
31 min
56: The Atomic Nucleus
In the first of two lectures on nuclear physics, study the atomic nucleus, which consists of positively charged protons and electrically neutral neutrons, held together by the strong nuclear force. Many combinations of protons and neutrons are unstable; such nuclei are radioactive and decay with characteristic half lives.
31 min
57: Energy from the Nucleus
Investigate nuclear fission, in which a heavy, unstable nucleus breaks apart; and nuclear fusion, where light nuclei are joined. In both, the released energy is millions of times greater than the energy from chemical reactions and comes from the conversion of nuclear binding energy to kinetic energy.
31 min
58: The Particle Zoo
By 1960 a myriad of seeming elementary particles had been discovered. Survey the standard model that restored order to this subatomic chaos, describing a universe whose fundamental particles include six quarks; the electron and two heavier cousins; elusive neutrinos; and force-carrying particles such as the photon.
30 min
59: An Evolving Universe
Trace the discoveries that led astronomers to conclude that the universe began some 14 billion years ago in a big bang. Detailed measurements of the cosmic microwave background and other observations point to an initial period of tremendous inflation, followed by slow expansion and an as-yet inexplicable accelerating phase.
31 min
60: Humble Physics-What We Don't Know
Having covered the remarkable discoveries in physics, turn to the great gap in our current knowledge, namely the nature of the dark matter and dark energy that constitute more than 95% of the universe. Close with a look at other mysteries that physicists are now working to solve.
32 min
