Astronomy 101 from Skynet University

Video Lectures

Displaying all 52 video lectures.
Lecture 1
Size and Scale
Play Video
Size and Scale
Topic: Size and Scale

Next:  Constellations and the Celestial Sphere (http://youtu.be/hGoBe3J0SJM)
Previous: Orientation (http://youtu.be/KtJdCgs1Dkk)

In Lesson 1, we explore the apparent motions of the stars, the sun, and the moon. We explain the apparent motions of the stars and the sun in terms of the motions of Earth: its daily spin on its axis, its annual orbit around the sun, and the long-term precession of its spin axis. We learn how length of day and the height of the sun in the sky at midday vary with season and latitude. We explore lunar phases, lunar and solar eclipses, and the cycle over which all eclipses repeat.
Lecture 2
Constellations and the Celestial Sphere
Play Video
Constellations and the Celestial Sphere
Topic: Constellations and the Celestial Sphere

Next: Motion of the Celestial Sphere (http://youtu.be/n_UeZ0-XDdU)
Previous: Size and Scale (http://youtu.be/Zbg-w2liDJI)

Related Lab: Introduction to Skynet (http://youtu.be/qDCQN1HtywY)

In Lesson 1, we explore the apparent motions of the stars, the sun, and the moon. We explain the apparent motions of the stars and the sun in terms of the motions of Earth: its daily spin on its axis, its annual orbit around the sun, and the long-term precession of its spin axis. We learn how length of day and the height of the sun in the sky at midday vary with season and latitude. We explore lunar phases, lunar and solar eclipses, and the cycle over which all eclipses repeat.
Lecture 3
Motion of the Celestial Sphere
Play Video
Motion of the Celestial Sphere
Topic: Motion of the Celestial Sphere

Next: Sun-Earth-Moon Scale Model (http://youtu.be/ksLErDRXFi8)
Previous: Constellations and the Celestial Sphere (http://youtu.be/hGoBe3J0SJM)

In Lesson 1, we explore the apparent motions of the stars, the sun, and the moon. We explain the apparent motions of the stars and the sun in terms of the motions of Earth: its daily spin on its axis, its annual orbit around the sun, and the long-term precession of its spin axis. We learn how length of day and the height of the sun in the sky at midday vary with season and latitude. We explore lunar phases, lunar and solar eclipses, and the cycle over which all eclipses repeat.
Lecture 4
Sun-Earth-Moon Scale Model
Play Video
Sun-Earth-Moon Scale Model
Topic: Sun-Earth-Moon Scale Model

Next: Solar vs. Sidereal Time (http://youtu.be/3ncrEEiwlvc)
Previous: Motion of the Celestial Sphere (http://youtu.be/n_UeZ0-XDdU)

In Lesson 1, we explore the apparent motions of the stars, the sun, and the moon. We explain the apparent motions of the stars and the sun in terms of the motions of Earth: its daily spin on its axis, its annual orbit around the sun, and the long-term precession of its spin axis. We learn how length of day and the height of the sun in the sky at midday vary with season and latitude. We explore lunar phases, lunar and solar eclipses, and the cycle over which all eclipses repeat.
Lecture 5
Solar vs. Sidereal Time
Play Video
Solar vs. Sidereal Time
Topic: Solar vs. Sidereal Time

Next: Seasons (http://youtu.be/Kg7N95cOgeA)
Previous: Sun-Earth-Moon Scale Model (http://youtu.be/ksLErDRXFi8)

In Lesson 1, we explore the apparent motions of the stars, the sun, and the moon. We explain the apparent motions of the stars and the sun in terms of the motions of Earth: its daily spin on its axis, its annual orbit around the sun, and the long-term precession of its spin axis. We learn how length of day and the height of the sun in the sky at midday vary with season and latitude. We explore lunar phases, lunar and solar eclipses, and the cycle over which all eclipses repeat.
Lecture 6
Seasons
Play Video
Seasons
Topic: Seasons

Next: Precession (http://youtu.be/kSYlNr8uKB8)
Previous: Solar vs. Sidereal Time (http://youtu.be/3ncrEEiwlvc)

Related Lab: Earth and the Seasons
(Globe Version: http://youtu.be/Z3tvQ5ohGTM)
(Stellarium Version: http://youtu.be/o1P_JMA0D0w)

In Lesson 1, we explore the apparent motions of the stars, the sun, and the moon. We explain the apparent motions of the stars and the sun in terms of the motions of Earth: its daily spin on its axis, its annual orbit around the sun, and the long-term precession of its spin axis. We learn how length of day and the height of the sun in the sky at midday vary with season and latitude. We explore lunar phases, lunar and solar eclipses, and the cycle over which all eclipses repeat.
Lecture 7
Precession
Play Video
Precession
Topic: Precession

Next: Lunar Phases (http://youtu.be/QBEyJ4_j9Ts)
Previous: Seasons (http://youtu.be/Kg7N95cOgeA)

In Lesson 1, we explore the apparent motions of the stars, the sun, and the moon. We explain the apparent motions of the stars and the sun in terms of the motions of Earth: its daily spin on its axis, its annual orbit around the sun, and the long-term precession of its spin axis. We learn how length of day and the height of the sun in the sky at midday vary with season and latitude. We explore lunar phases, lunar and solar eclipses, and the cycle over which all eclipses repeat.
Lecture 8
Lunar Phases
Play Video
Lunar Phases
Topic: Lunar Phases

Next: Lunar Month (http://youtu.be/PZXM89zQw5I)
Previous: Precession (http://youtu.be/kSYlNr8uKB8)

In Lesson 1, we explore the apparent motions of the stars, the sun, and the moon. We explain the apparent motions of the stars and the sun in terms of the motions of Earth: its daily spin on its axis, its annual orbit around the sun, and the long-term precession of its spin axis. We learn how length of day and the height of the sun in the sky at midday vary with season and latitude. We explore lunar phases, lunar and solar eclipses, and the cycle over which all eclipses repeat.
Lecture 9
Lunar Month
Play Video
Lunar Month
Topic: Lunar Month

Next: Eclipses (http://youtu.be/bZEbl-oryP8)
Previous: Lunar Phases (http://youtu.be/QBEyJ4_j9Ts)

In Lesson 1, we explore the apparent motions of the stars, the sun, and the moon. We explain the apparent motions of the stars and the sun in terms of the motions of Earth: its daily spin on its axis, its annual orbit around the sun, and the long-term precession of its spin axis. We learn how length of day and the height of the sun in the sky at midday vary with season and latitude. We explore lunar phases, lunar and solar eclipses, and the cycle over which all eclipses repeat.
Lecture 10
Eclipses
Play Video
Eclipses
Topic: Eclipses

Next: Eclipse Seasons (http://youtu.be/kh7VljWmcUM)
Previous: Lunar Month (http://youtu.be/PZXM89zQw5I)

In Lesson 1, we explore the apparent motions of the stars, the sun, and the moon. We explain the apparent motions of the stars and the sun in terms of the motions of Earth: its daily spin on its axis, its annual orbit around the sun, and the long-term precession of its spin axis. We learn how length of day and the height of the sun in the sky at midday vary with season and latitude. We explore lunar phases, lunar and solar eclipses, and the cycle over which all eclipses repeat.
Lecture 11
Eclipse Seasons
Play Video
Eclipse Seasons
Topic: Eclipse Seasons

Next: Saros Cycle (http://youtu.be/35aJduq8PIs)
Previous: Eclipses (http://youtu.be/bZEbl-oryP8)

In Lesson 1, we explore the apparent motions of the stars, the sun, and the moon. We explain the apparent motions of the stars and the sun in terms of the motions of Earth: its daily spin on its axis, its annual orbit around the sun, and the long-term precession of its spin axis. We learn how length of day and the height of the sun in the sky at midday vary with season and latitude. We explore lunar phases, lunar and solar eclipses, and the cycle over which all eclipses repeat.
Lecture 12
Saros Cycle
Play Video
Saros Cycle
Topic: Saros Cycle

Next: Lesson 2 (http://www.youtube.com/playlist?list=PLE25EA806E9A420B2)
Previous: Eclipse Seasons (http://youtu.be/kh7VljWmcUM)

In Lesson 1, we explore the apparent motions of the stars, the sun, and the moon. We explain the apparent motions of the stars and the sun in terms of the motions of Earth: its daily spin on its axis, its annual orbit around the sun, and the long-term precession of its spin axis. We learn how length of day and the height of the sun in the sky at midday vary with season and latitude. We explore lunar phases, lunar and solar eclipses, and the cycle over which all eclipses repeat.
Lecture 13
Stonehenge
Play Video
Stonehenge
Topic: Stonehenge

Next:  Geocentric Models (http://youtu.be/oJ51wyoth4Q)
Previous: Lesson 1 (http://www.youtube.com/playlist?list=PL9D50FACE21694A26)

In Lesson 2, we explore the apparent motions of the planets, as well as attempts to explain these motions throughout history. Specifically, we explore the geocentric models of Aristotle and Ptolemy and the heliocentric models Aristarchus, Copernicus, and Kepler, culminating in Kepler's three laws of planetary motion. We explore tests of these models by Galileo and others. Finally, we learn how Newton explained Kepler's empirical laws with physical law and universal law. But we begin by exploring Stonehenge as an example pre-written-history astronomy, or archaeoastronomy.
Lecture 14
Geocentric Models
Play Video
Geocentric Models
Topic: Geocentric Models

Next:  Heliocentric Models (http://youtu.be/fJVEHI3uOtw)
Previous: Stonehenge (http://youtu.be/nc3sEAZ-dhg)

In Lesson 2, we explore the apparent motions of the planets, as well as attempts to explain these motions throughout history. Specifically, we explore the geocentric models of Aristotle and Ptolemy and the heliocentric models Aristarchus, Copernicus, and Kepler, culminating in Kepler's three laws of planetary motion. We explore tests of these models by Galileo and others. Finally, we learn how Newton explained Kepler's empirical laws with physical law and universal law. But we begin by exploring Stonehenge as an example pre-written-history astronomy, or archaeoastronomy.
Lecture 15
Heliocentric Models
Play Video
Heliocentric Models
Topic: Heliocentric Models

Next:  Galilean Revolution (http://youtu.be/i0ivBULSsdM)
Previous: Geocentric Models (http://youtu.be/oJ51wyoth4Q)

In Lesson 2, we explore the apparent motions of the planets, as well as attempts to explain these motions throughout history. Specifically, we explore the geocentric models of Aristotle and Ptolemy and the heliocentric models Aristarchus, Copernicus, and Kepler, culminating in Kepler's three laws of planetary motion. We explore tests of these models by Galileo and others. Finally, we learn how Newton explained Kepler's empirical laws with physical law and universal law. But we begin by exploring Stonehenge as an example pre-written-history astronomy, or archaeoastronomy.
Lecture 16
Galilean Revolution
Play Video
Galilean Revolution
Topic: Galilean Revolution

Next: Aberration of Starlight and Stellar Parallax (http://youtu.be/kqvBVC8hkTs)
Previous: Heliocentric Models (http://youtu.be/fJVEHI3uOtw)

Related Lab: Galilean Revolution (http://youtu.be/rolUwut4pX0)

In Lesson 2, we explore the apparent motions of the planets, as well as attempts to explain these motions throughout history. Specifically, we explore the geocentric models of Aristotle and Ptolemy and the heliocentric models Aristarchus, Copernicus, and Kepler, culminating in Kepler's three laws of planetary motion. We explore tests of these models by Galileo and others. Finally, we learn how Newton explained Kepler's empirical laws with physical law and universal law. But we begin by exploring Stonehenge as an example pre-written-history astronomy, or archaeoastronomy.
Lecture 17
Aberration of Starlight and Stellar Parallax
Play Video
Aberration of Starlight and Stellar Parallax
Topic: Aberration of Starlight and Stellar Parallax

Next: Tycho and Kepler (http://youtu.be/dMnSL4jk5tU)
Previous: Galilean Revolution (http://youtu.be/i0ivBULSsdM)

Related Lab: Parallax (http://youtu.be/FdIOAFhGYos)

In Lesson 2, we explore the apparent motions of the planets, as well as attempts to explain these motions throughout history. Specifically, we explore the geocentric models of Aristotle and Ptolemy and the heliocentric models Aristarchus, Copernicus, and Kepler, culminating in Kepler's three laws of planetary motion. We explore tests of these models by Galileo and others. Finally, we learn how Newton explained Kepler's empirical laws with physical law and universal law. But we begin by exploring Stonehenge as an example pre-written-history astronomy, or archaeoastronomy.

YouTube Channel: http://www.youtube.com/introastro
Lecture 18
Tycho and Kepler
Play Video
Tycho and Kepler
Topic: Tycho and Kepler

Next: Kepler's Laws of Planetary Motion (http://youtu.be/Kyvhonwu9Ss)
Previous: Aberration of Starlight and Stellar Parallax (http://youtu.be/kqvBVC8hkTs)

Related Lab: Parallax (http://youtu.be/FdIOAFhGYos)

In Lesson 2, we explore the apparent motions of the planets, as well as attempts to explain these motions throughout history. Specifically, we explore the geocentric models of Aristotle and Ptolemy and the heliocentric models Aristarchus, Copernicus, and Kepler, culminating in Kepler's three laws of planetary motion. We explore tests of these models by Galileo and others. Finally, we learn how Newton explained Kepler's empirical laws with physical law and universal law. But we begin by exploring Stonehenge as an example pre-written-history astronomy, or archaeoastronomy.
Lecture 19
Kepler's Laws of Planetary Motion
Play Video
Kepler's Laws of Planetary Motion
Topic: Kepler's Laws of Planetary Motion

Next: Measuring the Astronomical Unit (http://youtu.be/AROp4EhWnhc)
Previous: Tycho and Kepler (http://youtu.be/dMnSL4jk5tU)

Related Lab: Galilean Revolution (http://youtu.be/rolUwut4pX0)

In Lesson 2, we explore the apparent motions of the planets, as well as attempts to explain these motions throughout history. Specifically, we explore the geocentric models of Aristotle and Ptolemy and the heliocentric models Aristarchus, Copernicus, and Kepler, culminating in Kepler's three laws of planetary motion. We explore tests of these models by Galileo and others. Finally, we learn how Newton explained Kepler's empirical laws with physical law and universal law. But we begin by exploring Stonehenge as an example pre-written-history astronomy, or archaeoastronomy.
Lecture 20
Measuring the Astronomical Unit
Play Video
Measuring the Astronomical Unit
Topic: Measuring the Astronomical Unit

Next: Newton's Laws of Motion (http://youtu.be/3HtwKhPcibc)
Previous: Kepler's Laws of Planetary Motion (http://youtu.be/Kyvhonwu9Ss)

Related Lab: Parallax (http://youtu.be/FdIOAFhGYos)

In Lesson 2, we explore the apparent motions of the planets, as well as attempts to explain these motions throughout history. Specifically, we explore the geocentric models of Aristotle and Ptolemy and the heliocentric models Aristarchus, Copernicus, and Kepler, culminating in Kepler's three laws of planetary motion. We explore tests of these models by Galileo and others. Finally, we learn how Newton explained Kepler's empirical laws with physical law and universal law. But we begin by exploring Stonehenge as an example pre-written-history astronomy, or archaeoastronomy.
Lecture 21
Newton's Laws of Motion
Play Video
Newton's Laws of Motion
Topic: Newton's Laws of Motion

Next: Newton's Law of Universal Gravitation (http://youtu.be/jBnM3kysssA)
Previous: Measuring the Astronomical Unit (http://youtu.be/AROp4EhWnhc)

In Lesson 2, we explore the apparent motions of the planets, as well as attempts to explain these motions throughout history. Specifically, we explore the geocentric models of Aristotle and Ptolemy and the heliocentric models Aristarchus, Copernicus, and Kepler, culminating in Kepler's three laws of planetary motion. We explore tests of these models by Galileo and others. Finally, we learn how Newton explained Kepler's empirical laws with physical law and universal law. But we begin by exploring Stonehenge as an example pre-written-history astronomy, or archaeoastronomy.
Lecture 22
Newton's Law of Universal Gravitation
Play Video
Newton's Law of Universal Gravitation
Topic: Newton's Law of Universal Gravitation

Next: Derivation of Kepler's Laws from Newton's Laws (http://youtu.be/zM2fqGsvwFQ)
Previous: Newton's Laws of Motion (http://youtu.be/3HtwKhPcibc)

In Lesson 2, we explore the apparent motions of the planets, as well as attempts to explain these motions throughout history. Specifically, we explore the geocentric models of Aristotle and Ptolemy and the heliocentric models Aristarchus, Copernicus, and Kepler, culminating in Kepler's three laws of planetary motion. We explore tests of these models by Galileo and others. Finally, we learn how Newton explained Kepler's empirical laws with physical law and universal law. But we begin by exploring Stonehenge as an example pre-written-history astronomy, or archaeoastronomy.
Lecture 23
Derivation of Kepler's Laws from Newton's Laws
Play Video
Derivation of Kepler's Laws from Newton's Laws
Topic: Derivation of Kepler's Laws from Newton's Laws

Next: Lesson 3 (http://www.youtube.com/playlist?list=PLy034wwN98YKWZ7rjMc7suhkiaDrh4Id4)
Previous: Newton's Law of Universal Gravitation (http://youtu.be/jBnM3kysssA)

Related Lab: Galilean Revolution (http://youtu.be/FdIOAFhGYos)

In Lesson 2, we explore the apparent motions of the planets, as well as attempts to explain these motions throughout history. Specifically, we explore the geocentric models of Aristotle and Ptolemy and the heliocentric models Aristarchus, Copernicus, and Kepler, culminating in Kepler's three laws of planetary motion. We explore tests of these models by Galileo and others. Finally, we learn how Newton explained Kepler's empirical laws with physical law and universal law. But we begin by exploring Stonehenge as an example pre-written-history astronomy, or archaeoastronomy.
Lecture 24
Light, Cosmic Rays, Neutrinos, and Gravitational Waves
Play Video
Light, Cosmic Rays, Neutrinos, and Gravitational Waves
Topic: Light, Cosmic Rays, Neutrinos, and Gravitational Waves

Next:  Particle vs. Wave Motion (http://youtu.be/45Ys5-1jFcI)
Previous: Lesson 2 (http://www.youtube.com/playlist?list=PLE25EA806E9A420B2)

In Lesson 3, we explore how we receive information from the universe, primarily in the form of light. We explore the nature of light, beginning with whether it is a particle or a wave. If it is a wave, what is the medium in which the wave travels? We explore how light is created, and study two examples in detail: thermal radiation and atomic absorption and emission lines. We study the absorption and emission lines of hydrogen, the most abundant element in the universe, in particular. We learn how all of this information can be used to measure compositions and temperatures. We explore the Doppler effect and how it can be used to measure line-of-sight velocities, internal motions, etc.
Lecture 25
Particle vs. Wave Motion
Play Video
Particle vs. Wave Motion
Topic: Particle vs. Wave Motion

Next:  Diffraction, Interference, and Polarization (http://youtu.be/xFrvL2r-YB8)
Previous: Light, Cosmic Rays, Neutrinos, and Gravitational Waves (http://youtu.be/kkGStNAAd_g)

In Lesson 3, we explore how we receive information from the universe, primarily in the form of light. We explore the nature of light, beginning with whether it is a particle or a wave. If it is a wave, what is the medium in which the wave travels? We explore how light is created, and study two examples in detail: thermal radiation and atomic absorption and emission lines. We study the absorption and emission lines of hydrogen, the most abundant element in the universe, in particular. We learn how all of this information can be used to measure compositions and temperatures. We explore the Doppler effect and how it can be used to measure line-of-sight velocities, internal motions, etc.
Lecture 26
Diffraction, Interference, and Polarization
Play Video
Diffraction, Interference, and Polarization
Topic: Diffraction, Interference, and Polarization

Next:  Electromagnetic Spectrum (http://youtu.be/6ylZgURxlmc)
Previous: Particle vs. Wave Motion (http://youtu.be/45Ys5-1jFcI)

In Lesson 3, we explore how we receive information from the universe, primarily in the form of light. We explore the nature of light, beginning with whether it is a particle or a wave. If it is a wave, what is the medium in which the wave travels? We explore how light is created, and study two examples in detail: thermal radiation and atomic absorption and emission lines. We study the absorption and emission lines of hydrogen, the most abundant element in the universe, in particular. We learn how all of this information can be used to measure compositions and temperatures. We explore the Doppler effect and how it can be used to measure line-of-sight velocities, internal motions, etc.
Lecture 27
Electromagnetic Spectrum
Play Video
Electromagnetic Spectrum
Topic: Electromagnetic Spectrum

Next:  Light and the Electromagnetic Field (http://youtu.be/UII2b5BTYGY)
Previous: Diffraction, Interference, and Polarization (http://youtu.be/xFrvL2r-YB8)

In Lesson 3, we explore how we receive information from the universe, primarily in the form of light. We explore the nature of light, beginning with whether it is a particle or a wave. If it is a wave, what is the medium in which the wave travels? We explore how light is created, and study two examples in detail: thermal radiation and atomic absorption and emission lines. We study the absorption and emission lines of hydrogen, the most abundant element in the universe, in particular. We learn how all of this information can be used to measure compositions and temperatures. We explore the Doppler effect and how it can be used to measure line-of-sight velocities, internal motions, etc.
Lecture 28
Light and the Electromagnetic Field
Play Video
Light and the Electromagnetic Field
Topic: Light and the Electromagnetic Field

Next:  Thermal Radiation (http://youtu.be/RiD8Rmx14U0)
Previous: Electromagnetic Spectrum (http://youtu.be/6ylZgURxlmc)

In Lesson 3, we explore how we receive information from the universe, primarily in the form of light. We explore the nature of light, beginning with whether it is a particle or a wave. If it is a wave, what is the medium in which the wave travels? We explore how light is created, and study two examples in detail: thermal radiation and atomic absorption and emission lines. We study the absorption and emission lines of hydrogen, the most abundant element in the universe, in particular. We learn how all of this information can be used to measure compositions and temperatures. We explore the Doppler effect and how it can be used to measure line-of-sight velocities, internal motions, etc.
Lecture 29
Thermal Radiation
Play Video
Thermal Radiation
Topic: Thermal Radiation

Next:  Why Are There No Green Stars? (http://youtu.be/KTZE9N82o9k)
Previous: Light and the Electromagnetic Field (http://youtu.be/UII2b5BTYGY)

In Lesson 3, we explore how we receive information from the universe, primarily in the form of light. We explore the nature of light, beginning with whether it is a particle or a wave. If it is a wave, what is the medium in which the wave travels? We explore how light is created, and study two examples in detail: thermal radiation and atomic absorption and emission lines. We study the absorption and emission lines of hydrogen, the most abundant element in the universe, in particular. We learn how all of this information can be used to measure compositions and temperatures. We explore the Doppler effect and how it can be used to measure line-of-sight velocities, internal motions, etc.
Lecture 30
Why Are There No Green Stars?
Play Video
Why Are There No Green Stars?
Topic: Why Are There No Green Stars?

Next:  Spectroscopy and Kirchhoff's Laws (http://youtu.be/HjVw8PKmtgA)
Previous: Thermal Radiation (http://youtu.be/RiD8Rmx14U0)

In Lesson 3, we explore how we receive information from the universe, primarily in the form of light. We explore the nature of light, beginning with whether it is a particle or a wave. If it is a wave, what is the medium in which the wave travels? We explore how light is created, and study two examples in detail: thermal radiation and atomic absorption and emission lines. We study the absorption and emission lines of hydrogen, the most abundant element in the universe, in particular. We learn how all of this information can be used to measure compositions and temperatures. We explore the Doppler effect and how it can be used to measure line-of-sight velocities, internal motions, etc.
Lecture 31
Spectroscopy and Kirchhoff's Laws
Play Video
Spectroscopy and Kirchhoff's Laws
Topic: Spectroscopy and Kirchhoff's Laws

Next:  Atomic Structure (http://youtu.be/1_18dmSgIqI)
Previous: Why Are There No Green Stars? (http://youtu.be/KTZE9N82o9k)

In Lesson 3, we explore how we receive information from the universe, primarily in the form of light. We explore the nature of light, beginning with whether it is a particle or a wave. If it is a wave, what is the medium in which the wave travels? We explore how light is created, and study two examples in detail: thermal radiation and atomic absorption and emission lines. We study the absorption and emission lines of hydrogen, the most abundant element in the universe, in particular. We learn how all of this information can be used to measure compositions and temperatures. We explore the Doppler effect and how it can be used to measure line-of-sight velocities, internal motions, etc.
Lecture 32
Atomic Structure
Play Video
Atomic Structure
Topic: Atomic Structure

Next:  Hydrogen Spectral Series (http://youtu.be/6bSpcr0927U)
Previous: Spectroscopy and Kirchhoff's Laws (http://youtu.be/HjVw8PKmtgA)

In Lesson 3, we explore how we receive information from the universe, primarily in the form of light. We explore the nature of light, beginning with whether it is a particle or a wave. If it is a wave, what is the medium in which the wave travels? We explore how light is created, and study two examples in detail: thermal radiation and atomic absorption and emission lines. We study the absorption and emission lines of hydrogen, the most abundant element in the universe, in particular. We learn how all of this information can be used to measure compositions and temperatures. We explore the Doppler effect and how it can be used to measure line-of-sight velocities, internal motions, etc.
Lecture 33
Hydrogen Spectral Series
Play Video
Hydrogen Spectral Series
Topic: Hydrogen Spectral Series

Next:  Kirchhoff's Laws Explained (http://youtu.be/IiLJYN2jduA)
Previous: Atomic Structure (http://youtu.be/1_18dmSgIqI)

In Lesson 3, we explore how we receive information from the universe, primarily in the form of light. We explore the nature of light, beginning with whether it is a particle or a wave. If it is a wave, what is the medium in which the wave travels? We explore how light is created, and study two examples in detail: thermal radiation and atomic absorption and emission lines. We study the absorption and emission lines of hydrogen, the most abundant element in the universe, in particular. We learn how all of this information can be used to measure compositions and temperatures. We explore the Doppler effect and how it can be used to measure line-of-sight velocities, internal motions, etc.
Lecture 34
Kirchhoff's Laws Explained
Play Video
Kirchhoff's Laws Explained
Topic: Kirchhoff's Laws Explained

Next:  Doppler Effect (http://youtu.be/vFNtV37m2a4)
Previous: Hydrogen Spectral Series (http://youtu.be/6bSpcr0927U)

In Lesson 3, we explore how we receive information from the universe, primarily in the form of light. We explore the nature of light, beginning with whether it is a particle or a wave. If it is a wave, what is the medium in which the wave travels? We explore how light is created, and study two examples in detail: thermal radiation and atomic absorption and emission lines. We study the absorption and emission lines of hydrogen, the most abundant element in the universe, in particular. We learn how all of this information can be used to measure compositions and temperatures. We explore the Doppler effect and how it can be used to measure line-of-sight velocities, internal motions, etc.
Lecture 35
Doppler Effect
Play Video
Doppler Effect
Topic: Doppler Effect

Next:  Spectral Line Widths (http://youtu.be/V-hiT43_YGo)
Previous: Kirchhoff's Laws Explained (http://youtu.be/IiLJYN2jduA)

Related Lab: Rotation Curve and Mass of the Galaxy

In Lesson 3, we explore how we receive information from the universe, primarily in the form of light. We explore the nature of light, beginning with whether it is a particle or a wave. If it is a wave, what is the medium in which the wave travels? We explore how light is created, and study two examples in detail: thermal radiation and atomic absorption and emission lines. We study the absorption and emission lines of hydrogen, the most abundant element in the universe, in particular. We learn how all of this information can be used to measure compositions and temperatures. We explore the Doppler effect and how it can be used to measure line-of-sight velocities, internal motions, etc.
Lecture 36
Spectral Line Widths
Play Video
Spectral Line Widths
Topic: Spectral Line Widths

Next:  Lesson 4 (https://www.youtube.com/playlist?list=PLy034wwN98YIcO0H7fiOzM0rlvtV7gpHj)
Previous: Doppler Effect (http://youtu.be/vFNtV37m2a4)

In Lesson 3, we explore how we receive information from the universe, primarily in the form of light. We explore the nature of light, beginning with whether it is a particle or a wave. If it is a wave, what is the medium in which the wave travels? We explore how light is created, and study two examples in detail: thermal radiation and atomic absorption and emission lines. We study the absorption and emission lines of hydrogen, the most abundant element in the universe, in particular. We learn how all of this information can be used to measure compositions and temperatures. We explore the Doppler effect and how it can be used to measure line-of-sight velocities, internal motions, etc.
Lecture 37
Basic Reflecting Telescope
Play Video
Basic Reflecting Telescope
Topic: Basic Reflecting Telescope

Next:  Basic Refracting Telescope (http://youtu.be/Tw_u43JFYow)
Previous: Lesson 3 (http://www.youtube.com/playlist?list=PLy034wwN98YKWZ7rjMc7suhkiaDrh4Id4)

In Lesson 4, we explore the technologies that astronomers have developed, and continue to develop, to detect light from the universe, at both visible and invisible wavelengths. At visible and near-visible wavelengths, we compare and contrast reflecting and refracting telescope designs, as well as detectors, including spectrographs. We explore why astronomers build bigger and bigger telescopes, and consider both design and atmospheric limitations. We explore technologies that are being developed to overcome atmospheric limitations -- to untwinkle the stars. We also explore how light is detected at radio wavelengths, which can be done from the ground, and at other wavelengths, which requires observing from space. We learn that a great deal can be gained by observing the same object at multiple wavelengths.
Lecture 38
Basic Refracting Telescope
Play Video
Basic Refracting Telescope
Topic: Basic Refracting Telescope

Next:  Reflecting vs. Refracting Telescopes (http://youtu.be/PcGNNhE5FXQ)
Previous: Basic Reflecting Telescope (http://youtu.be/JEr6MgW1qNI)

In Lesson 4, we explore the technologies that astronomers have developed, and continue to develop, to detect light from the universe, at both visible and invisible wavelengths. At visible and near-visible wavelengths, we compare and contrast reflecting and refracting telescope designs, as well as detectors, including spectrographs. We explore why astronomers build bigger and bigger telescopes, and consider both design and atmospheric limitations. We explore technologies that are being developed to overcome atmospheric limitations -- to untwinkle the stars. We also explore how light is detected at radio wavelengths, which can be done from the ground, and at other wavelengths, which requires observing from space. We learn that a great deal can be gained by observing the same object at multiple wavelengths.
Lecture 39
Reflecting vs. Refracting Telescopes
Play Video
Reflecting vs. Refracting Telescopes
Topic: Reflecting vs. Refracting Telescopes

Next:  Reflecting Telescope Designs (http://youtu.be/qYUsxSKSvUw)
Previous: Basic Refracting Telescope (http://youtu.be/Tw_u43JFYow)

In Lesson 4, we explore the technologies that astronomers have developed, and continue to develop, to detect light from the universe, at both visible and invisible wavelengths. At visible and near-visible wavelengths, we compare and contrast reflecting and refracting telescope designs, as well as detectors, including spectrographs. We explore why astronomers build bigger and bigger telescopes, and consider both design and atmospheric limitations. We explore technologies that are being developed to overcome atmospheric limitations -- to untwinkle the stars. We also explore how light is detected at radio wavelengths, which can be done from the ground, and at other wavelengths, which requires observing from space. We learn that a great deal can be gained by observing the same object at multiple wavelengths.
Lecture 40
Reflecting Telescope Designs
Play Video
Reflecting Telescope Designs
Topic: Reflecting Telescope Designs

Next:  Detectors (http://youtu.be/hT0Y91IT7bg)
Previous: Reflecting vs. Refracting Telescopes (http://youtu.be/PcGNNhE5FXQ)

In Lesson 4, we explore the technologies that astronomers have developed, and continue to develop, to detect light from the universe, at both visible and invisible wavelengths. At visible and near-visible wavelengths, we compare and contrast reflecting and refracting telescope designs, as well as detectors, including spectrographs. We explore why astronomers build bigger and bigger telescopes, and consider both design and atmospheric limitations. We explore technologies that are being developed to overcome atmospheric limitations -- to untwinkle the stars. We also explore how light is detected at radio wavelengths, which can be done from the ground, and at other wavelengths, which requires observing from space. We learn that a great deal can be gained by observing the same object at multiple wavelengths.
Lecture 41
Detectors
Play Video
Detectors
Topic: Detectors

Next:  Spectrographs (http://youtu.be/jAdRwsC78pQ)
Previous: Reflecting Telescope Designs (http://youtu.be/qYUsxSKSvUw)

In Lesson 4, we explore the technologies that astronomers have developed, and continue to develop, to detect light from the universe, at both visible and invisible wavelengths. At visible and near-visible wavelengths, we compare and contrast reflecting and refracting telescope designs, as well as detectors, including spectrographs. We explore why astronomers build bigger and bigger telescopes, and consider both design and atmospheric limitations. We explore technologies that are being developed to overcome atmospheric limitations -- to untwinkle the stars. We also explore how light is detected at radio wavelengths, which can be done from the ground, and at other wavelengths, which requires observing from space. We learn that a great deal can be gained by observing the same object at multiple wavelengths.
Lecture 42
Spectrographs
Play Video
Spectrographs
Topic: Spectrographs

Next:  Light-Gathering Power (http://youtu.be/IViqLwZlv3U)
Previous: Detectors (http://youtu.be/hT0Y91IT7bg)

In Lesson 4, we explore the technologies that astronomers have developed, and continue to develop, to detect light from the universe, at both visible and invisible wavelengths. At visible and near-visible wavelengths, we compare and contrast reflecting and refracting telescope designs, as well as detectors, including spectrographs. We explore why astronomers build bigger and bigger telescopes, and consider both design and atmospheric limitations. We explore technologies that are being developed to overcome atmospheric limitations -- to untwinkle the stars. We also explore how light is detected at radio wavelengths, which can be done from the ground, and at other wavelengths, which requires observing from space. We learn that a great deal can be gained by observing the same object at multiple wavelengths.
Lecture 43
Light-Gathering Power
Play Video
Light-Gathering Power
Topic: Light-Gathering Power

Next:  Resolving Power (http://youtu.be/9m5CpwfCmEI)
Previous:  Spectrographs (http://youtu.be/jAdRwsC78pQ)

In Lesson 4, we explore the technologies that astronomers have developed, and continue to develop, to detect light from the universe, at both visible and invisible wavelengths. At visible and near-visible wavelengths, we compare and contrast reflecting and refracting telescope designs, as well as detectors, including spectrographs. We explore why astronomers build bigger and bigger telescopes, and consider both design and atmospheric limitations. We explore technologies that are being developed to overcome atmospheric limitations -- to untwinkle the stars. We also explore how light is detected at radio wavelengths, which can be done from the ground, and at other wavelengths, which requires observing from space. We learn that a great deal can be gained by observing the same object at multiple wavelengths.
Lecture 44
Resolving Power
Play Video
Resolving Power
Topic: Resolving Power

Next:  Atmospheric Blurring (http://youtu.be/kqQ9rQ-VDdA)
Previous:  Light-Gathering Power (http://youtu.be/IViqLwZlv3U)

In Lesson 4, we explore the technologies that astronomers have developed, and continue to develop, to detect light from the universe, at both visible and invisible wavelengths. At visible and near-visible wavelengths, we compare and contrast reflecting and refracting telescope designs, as well as detectors, including spectrographs. We explore why astronomers build bigger and bigger telescopes, and consider both design and atmospheric limitations. We explore technologies that are being developed to overcome atmospheric limitations -- to untwinkle the stars. We also explore how light is detected at radio wavelengths, which can be done from the ground, and at other wavelengths, which requires observing from space. We learn that a great deal can be gained by observing the same object at multiple wavelengths.
Lecture 45
Atmospheric Blurring
Play Video
Atmospheric Blurring
Topic: Atmospheric Blurring

Next:  High-Resolution Observing (http://youtu.be/l28F6z46lK8)
Previous:  Resolving Power (http://youtu.be/9m5CpwfCmEI)

In Lesson 4, we explore the technologies that astronomers have developed, and continue to develop, to detect light from the universe, at both visible and invisible wavelengths. At visible and near-visible wavelengths, we compare and contrast reflecting and refracting telescope designs, as well as detectors, including spectrographs. We explore why astronomers build bigger and bigger telescopes, and consider both design and atmospheric limitations. We explore technologies that are being developed to overcome atmospheric limitations -- to untwinkle the stars. We also explore how light is detected at radio wavelengths, which can be done from the ground, and at other wavelengths, which requires observing from space. We learn that a great deal can be gained by observing the same object at multiple wavelengths.
Lecture 46
High-Resolution Observing
Play Video
High-Resolution Observing
Topic: High-Resolution Observing

Next:  University of North Carolina's Telescopes (http://youtu.be/xsYaAIpbMkM)
Previous:  Atmospheric Blurring (http://youtu.be/kqQ9rQ-VDdA)

In Lesson 4, we explore the technologies that astronomers have developed, and continue to develop, to detect light from the universe, at both visible and invisible wavelengths. At visible and near-visible wavelengths, we compare and contrast reflecting and refracting telescope designs, as well as detectors, including spectrographs. We explore why astronomers build bigger and bigger telescopes, and consider both design and atmospheric limitations. We explore technologies that are being developed to overcome atmospheric limitations -- to untwinkle the stars. We also explore how light is detected at radio wavelengths, which can be done from the ground, and at other wavelengths, which requires observing from space. We learn that a great deal can be gained by observing the same object at multiple wavelengths.
Lecture 47
University of North Carolina's Telescopes
Play Video
University of North Carolina's Telescopes
Topic: University of North Carolina's Telescopes

Next:  Jansky and Reber (http://youtu.be/QD_9ueCtwkg)
Previous:  High-Resolution Observing (http://youtu.be/l28F6z46lK8)

In Lesson 4, we explore the technologies that astronomers have developed, and continue to develop, to detect light from the universe, at both visible and invisible wavelengths. At visible and near-visible wavelengths, we compare and contrast reflecting and refracting telescope designs, as well as detectors, including spectrographs. We explore why astronomers build bigger and bigger telescopes, and consider both design and atmospheric limitations. We explore technologies that are being developed to overcome atmospheric limitations -- to untwinkle the stars. We also explore how light is detected at radio wavelengths, which can be done from the ground, and at other wavelengths, which requires observing from space. We learn that a great deal can be gained by observing the same object at multiple wavelengths.
Lecture 48
Jansky and Reber
Play Video
Jansky and Reber
Topic: Jansky and Reber

Next:  Radio Telescopes (http://youtu.be/Ftt8pEhnu7Y)
Previous:  University of North Carolina's Telescopes (http://youtu.be/xsYaAIpbMkM)

In Lesson 4, we explore the technologies that astronomers have developed, and continue to develop, to detect light from the universe, at both visible and invisible wavelengths. At visible and near-visible wavelengths, we compare and contrast reflecting and refracting telescope designs, as well as detectors, including spectrographs. We explore why astronomers build bigger and bigger telescopes, and consider both design and atmospheric limitations. We explore technologies that are being developed to overcome atmospheric limitations -- to untwinkle the stars. We also explore how light is detected at radio wavelengths, which can be done from the ground, and at other wavelengths, which requires observing from space. We learn that a great deal can be gained by observing the same object at multiple wavelengths.
Lecture 49
Radio Telescopes
Play Video
Radio Telescopes
Topic: Radio Telescopes

Next:  Radio Interferometers (http://youtu.be/7gja8u8kDi4)
Previous:  Jansky and Reber (http://youtu.be/QD_9ueCtwkg)

In Lesson 4, we explore the technologies that astronomers have developed, and continue to develop, to detect light from the universe, at both visible and invisible wavelengths. At visible and near-visible wavelengths, we compare and contrast reflecting and refracting telescope designs, as well as detectors, including spectrographs. We explore why astronomers build bigger and bigger telescopes, and consider both design and atmospheric limitations. We explore technologies that are being developed to overcome atmospheric limitations -- to untwinkle the stars. We also explore how light is detected at radio wavelengths, which can be done from the ground, and at other wavelengths, which requires observing from space. We learn that a great deal can be gained by observing the same object at multiple wavelengths.
Lecture 50
Radio Interferometers
Play Video
Radio Interferometers
Topic: Radio Interferometers

Next:  Introduction to Radio Astronomy (http://youtu.be/jCgv7yiSLMQ)
Previous:  Radio Telescopes (http://youtu.be/Ftt8pEhnu7Y)

In Lesson 4, we explore the technologies that astronomers have developed, and continue to develop, to detect light from the universe, at both visible and invisible wavelengths. At visible and near-visible wavelengths, we compare and contrast reflecting and refracting telescope designs, as well as detectors, including spectrographs. We explore why astronomers build bigger and bigger telescopes, and consider both design and atmospheric limitations. We explore technologies that are being developed to overcome atmospheric limitations -- to untwinkle the stars. We also explore how light is detected at radio wavelengths, which can be done from the ground, and at other wavelengths, which requires observing from space. We learn that a great deal can be gained by observing the same object at multiple wavelengths.
Lecture 51
Introduction to Radio Astronomy
Play Video
Introduction to Radio Astronomy
Topic: Introduction to Radio Astronomy

Next: Space-Based Telescopes (http://youtu.be/oUFTlt7LJB0)
Previous:  Radio Interferometers (http://youtu.be/7gja8u8kDi4)

In Lesson 4, we explore the technologies that astronomers have developed, and continue to develop, to detect light from the universe, at both visible and invisible wavelengths. At visible and near-visible wavelengths, we compare and contrast reflecting and refracting telescope designs, as well as detectors, including spectrographs. We explore why astronomers build bigger and bigger telescopes, and consider both design and atmospheric limitations. We explore technologies that are being developed to overcome atmospheric limitations -- to untwinkle the stars. We also explore how light is detected at radio wavelengths, which can be done from the ground, and at other wavelengths, which requires observing from space. We learn that a great deal can be gained by observing the same object at multiple wavelengths.
Lecture 52
Space-Based Telescopes
Play Video
Space-Based Telescopes
Topic: Space-Based Telescopes

Next: Lesson 5
Previous:  Introduction to Radio Astronomy (http://youtu.be/jCgv7yiSLMQ)

In Lesson 4, we explore the technologies that astronomers have developed, and continue to develop, to detect light from the universe, at both visible and invisible wavelengths. At visible and near-visible wavelengths, we compare and contrast reflecting and refracting telescope designs, as well as detectors, including spectrographs. We explore why astronomers build bigger and bigger telescopes, and consider both design and atmospheric limitations. We explore technologies that are being developed to overcome atmospheric limitations -- to untwinkle the stars. We also explore how light is detected at radio wavelengths, which can be done from the ground, and at other wavelengths, which requires observing from space. We learn that a great deal can be gained by observing the same object at multiple wavelengths.