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Subject:	Astronomy
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University of North Carolina at Chapel Hill

Name:	University of North Carolina at Chapel Hill (UNC)
Type:	University

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Astronomy 101 from Skynet University

Video Lectures

Displaying all 52 video lectures.

Lecture 1 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 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 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 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 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 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 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 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 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 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 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 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 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 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 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 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 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 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 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 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 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 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 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 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 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 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 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 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 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 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 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 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 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 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 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 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 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 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 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 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 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 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 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 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 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 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 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 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 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.