http://www.physicsbook.gatech.edu/api.php?action=feedcontributions&feedformat=atom&user=Edcunha3 2026-04-29T01:35:05Z User contributions MediaWiki 1.42.7 http://www.physicsbook.gatech.edu/index.php?title=Subrahmanyan_Chandrasekhar&diff=18041 2015-12-06T01:41:49Z

<p>Edcunha3: </p> <hr /> <div>Claimed by Ethan DCunha edcunha3<br /> <br /> Subrahmanyan Chandrasekhar was an Indian American astrophysicist born in Lahore, Punjab. Chandrasekhar was awarded, along with William A. Fowler, the 1983 Nobel Prize for Physics, with Chandrasekhar cited for his mathematical theory of the physical processes of importance to the structure and evolution of the stars. This work led to the currently accepted theory on the later evolutionary stages of massive stars, including black holes.<br /> <br /> Subrahmanyan Chandrasekhar was one of the foremost astrophysicists of the twentieth century. He was one of the first scientists to couple the study of physics with the study of astronomy. Chandra proved that there was an upper limit to the mass of a white dwarf. This limit, known as the Chandra limit, showed that stars more massive than the Sun would explode or form black holes as they died. Chandra also developed theories on star atmospheres, black holes, the illumination of the sunlit sky, star structures and star mass. In 1983 Chandra was awarded the Nobel Prize in Physics for his work on the physical processes involved in the structure and evolution of stars. Chandra published ten books and served as the editor of the prominent Astrophysical Journal for nineteen years. In 1999, four years after his death in August of 1995, NASA launched Chandra, a x-ray observatory named in honor of Subrahmanyan Chandrasekhar. The observatory studies the universe in the x-ray portion of the electromagnetic spectrum.<br /> <br /> [[File:Chandu.jpg|200px|thumb|left|alt text]] <br /> <br /> <br /> == Life and Education ==<br /> <br /> Chandrasekhar was born on 19 October 1910 in Lahore, Punjab, India in a Tamil family. At first he was tutored at home by his parents. Later, he attended Hindu High School in Madras to complete his high school education. Consequently, he attended Presidency College in Madras where he obtained his bachelors degree in physics. During this time, he published his first paper &quot;The Compton Scattering and the New Statistics&quot;. After completing his undergraduate studies, he was awarded a scholarship by the govenrment of India. Using this, he was able to pursue his graduate studies in University of Cambridge, under the guidance of professor R. H. Fowler. <br /> <br /> After receiving a bronze medal for his work on degenerate stars, in the summer of 1933, Chandrasekhar was awarded his PhD degree at Cambridge with a thesis among his four papers on rotating self-gravitating polytropes, and the following October, he was elected to a Prize Fellowship at Trinity College for the period 1933–1937.<br /> <br /> == Publications ==<br /> <br /> Chandrasekhar, S. (1958) [1939]. An Introduction to the Study of Stellar Structure. New York: Dover. ISBN 0-486-60413-6.<br /> <br /> Chandrasekhar, S. (2005) [1942]. Principles of Stellar Dynamics. New York: Dover. ISBN 0-486-44273-X.<br /> <br /> Chandrasekhar, S. (1960) [1950]. Radiative Transfer. New York: Dover. ISBN 0-486-60590-6.<br /> <br /> Chandrasekhar, S. (1975) [1960]. Plasma Physics. Chicago: The University of Chicago Press. ISBN 0-226-10084-7.<br /> <br /> Chandrasekhar, S. (1981) [1961]. Hydrodynamic and Hydromagnetic Stability. New York: Dover. ISBN 0-486-64071-X.<br /> <br /> Chandrasekhar, S. (1987) [1969]. Ellipsoidal Figures of Equilibrium. New York: Dover. ISBN 0-486-65258-0.<br /> <br /> Chandrasekhar, S. (1998) [1983]. The Mathematical Theory of Black Holes. New York: Oxford University Press. ISBN 0-19-850370-9.<br /> <br /> Chandrasekhar, S. (1990) [1987]. Truth and Beauty. Aesthetics and Motivations in Science. Chicago: The University of Chicago Press. ISBN 0-226-10087-1.<br /> <br /> Chandrasekhar, S. (1995). Newton's Principia for the Common Reader. Oxford: Clarendon Press. ISBN 0-19-851744-0.<br /> <br /> <br /> == Nobel Prize ==<br /> <br /> The Nobel Prize in Physics 1983 was divided equally between Subramanyan Chandrasekhar &quot;for his theoretical studies of the physical processes of importance to the structure and evolution of the stars&quot; and William Alfred Fowler &quot;for his theoretical and experimental studies of the nuclear reactions of importance in the formation of the chemical elements in the universe&quot;.<br /> <br /> <br /> == Chandrasekhar limit ==<br /> <br /> This was considered to be his greatest contribution to the world of physics. It is based on theories of black holes and dwarf stars. It is important to the field of astrophysics.<br /> <br /> Using Albert Einstein’s special theory of relativity and the principles of quantum physics, Chandrasekhar showed that it is impossible for a white dwarf star, which is supported solely by a degenerate gas of electrons, to be stable if its mass is greater than 1.44 times the mass of the Sun. If such a star does not completely exhaust its thermonuclear fuel, then this limiting mass may be slightly larger.<br /> <br /> All direct mass determinations of actual white dwarf stars have resulted in masses less than the Chandrasekhar limit. A star that ends its nuclear-burning lifetime with a mass greater than the Chandrasekhar limit must become either a neutron star or a black hole.<br /> <br /> [[File:Chandralimit.jpg|200px|thumb|left|alt text]] <br /> <br /> <br /> == References ==<br /> <br /> https://en.wikipedia.org/wiki/Subrahmanyan_Chandrasekhar<br /> <br /> http://starchild.gsfc.nasa.gov/docs/StarChild/whos_who_level2/chandra.html</div>

Edcunha3 http://www.physicsbook.gatech.edu/index.php?title=Subrahmanyan_Chandrasekhar&diff=18004 2015-12-06T01:37:36Z

<p>Edcunha3: </p> <hr /> <div>Claimed by Ethan DCunha edcunha3<br /> <br /> Subrahmanyan Chandrasekhar was an Indian American astrophysicist born in Lahore, Punjab. Chandrasekhar was awarded, along with William A. Fowler, the 1983 Nobel Prize for Physics, with Chandrasekhar cited for his mathematical theory of the physical processes of importance to the structure and evolution of the stars. This work led to the currently accepted theory on the later evolutionary stages of massive stars, including black holes.<br /> <br /> Subrahmanyan Chandrasekhar was one of the foremost astrophysicists of the twentieth century. He was one of the first scientists to couple the study of physics with the study of astronomy. Chandra proved that there was an upper limit to the mass of a white dwarf. This limit, known as the Chandra limit, showed that stars more massive than the Sun would explode or form black holes as they died. Chandra also developed theories on star atmospheres, black holes, the illumination of the sunlit sky, star structures and star mass. In 1983 Chandra was awarded the Nobel Prize in Physics for his work on the physical processes involved in the structure and evolution of stars. Chandra published ten books and served as the editor of the prominent Astrophysical Journal for nineteen years. In 1999, four years after his death in August of 1995, NASA launched Chandra, a x-ray observatory named in honor of Subrahmanyan Chandrasekhar. The observatory studies the universe in the x-ray portion of the electromagnetic spectrum.<br /> <br /> [[File:Chandu.jpg|200px|thumb|left|alt text]] <br /> <br /> <br /> == Life and Education ==<br /> <br /> Chandrasekhar was born on 19 October 1910 in Lahore, Punjab, India in a Tamil family. At first he was tutored at home by his parents. Later, he attended Hindu High School in Madras to complete his high school education. Consequently, he attended Presidency College in Madras where he obtained his bachelors degree in physics. During this time, he published his first paper &quot;The Compton Scattering and the New Statistics&quot;. After completing his undergraduate studies, he was awarded a scholarship by the govenrment of India. Using this, he was able to pursue his graduate studies in University of Cambridge, under the guidance of professor R. H. Fowler. <br /> <br /> After receiving a bronze medal for his work on degenerate stars, in the summer of 1933, Chandrasekhar was awarded his PhD degree at Cambridge with a thesis among his four papers on rotating self-gravitating polytropes, and the following October, he was elected to a Prize Fellowship at Trinity College for the period 1933–1937.<br /> <br /> == Publications ==<br /> <br /> Chandrasekhar, S. (1958) [1939]. An Introduction to the Study of Stellar Structure. New York: Dover. ISBN 0-486-60413-6.<br /> <br /> Chandrasekhar, S. (2005) [1942]. Principles of Stellar Dynamics. New York: Dover. ISBN 0-486-44273-X.<br /> <br /> Chandrasekhar, S. (1960) [1950]. Radiative Transfer. New York: Dover. ISBN 0-486-60590-6.<br /> <br /> Chandrasekhar, S. (1975) [1960]. Plasma Physics. Chicago: The University of Chicago Press. ISBN 0-226-10084-7.<br /> <br /> Chandrasekhar, S. (1981) [1961]. Hydrodynamic and Hydromagnetic Stability. New York: Dover. ISBN 0-486-64071-X.<br /> <br /> Chandrasekhar, S. (1987) [1969]. Ellipsoidal Figures of Equilibrium. New York: Dover. ISBN 0-486-65258-0.<br /> <br /> Chandrasekhar, S. (1998) [1983]. The Mathematical Theory of Black Holes. New York: Oxford University Press. ISBN 0-19-850370-9.<br /> <br /> Chandrasekhar, S. (1990) [1987]. Truth and Beauty. Aesthetics and Motivations in Science. Chicago: The University of Chicago Press. ISBN 0-226-10087-1.<br /> <br /> Chandrasekhar, S. (1995). Newton's Principia for the Common Reader. Oxford: Clarendon Press. ISBN 0-19-851744-0.<br /> <br /> <br /> == Nobel Prize ==<br /> <br /> The Nobel Prize in Physics 1983 was divided equally between Subramanyan Chandrasekhar &quot;for his theoretical studies of the physical processes of importance to the structure and evolution of the stars&quot; and William Alfred Fowler &quot;for his theoretical and experimental studies of the nuclear reactions of importance in the formation of the chemical elements in the universe&quot;.<br /> <br /> <br /> == Chandrasekhar limit ==<br /> <br /> This was considered to be his greatest contribution to the world of physics. It is based on theories of black holes and dwarf stars. It is important to the field of astrophysics.<br /> <br /> Using Albert Einstein’s special theory of relativity and the principles of quantum physics, Chandrasekhar showed that it is impossible for a white dwarf star, which is supported solely by a degenerate gas of electrons, to be stable if its mass is greater than 1.44 times the mass of the Sun. If such a star does not completely exhaust its thermonuclear fuel, then this limiting mass may be slightly larger.<br /> <br /> All direct mass determinations of actual white dwarf stars have resulted in masses less than the Chandrasekhar limit. A star that ends its nuclear-burning lifetime with a mass greater than the Chandrasekhar limit must become either a neutron star or a black hole.<br /> <br /> [[File:Chandralimit.jpg|200px|thumb|left|alt text]] <br /> <br /> <br /> == References ==<br /> <br /> https://en.wikipedia.org/wiki/Subrahmanyan_Chandrasekhar<br /> http://starchild.gsfc.nasa.gov/docs/StarChild/whos_who_level2/chandra.html</div>

Edcunha3 http://www.physicsbook.gatech.edu/index.php?title=Subrahmanyan_Chandrasekhar&diff=18003 2015-12-06T01:37:05Z

<p>Edcunha3: </p> <hr /> <div>Claimed by Ethan DCunha edcunha3<br /> <br /> Subrahmanyan Chandrasekhar was an Indian American astrophysicist born in Lahore, Punjab. Chandrasekhar was awarded, along with William A. Fowler, the 1983 Nobel Prize for Physics, with Chandrasekhar cited for his mathematical theory of the physical processes of importance to the structure and evolution of the stars. This work led to the currently accepted theory on the later evolutionary stages of massive stars, including black holes.<br /> <br /> Subrahmanyan Chandrasekhar was one of the foremost astrophysicists of the twentieth century. He was one of the first scientists to couple the study of physics with the study of astronomy. Chandra proved that there was an upper limit to the mass of a white dwarf. This limit, known as the Chandra limit, showed that stars more massive than the Sun would explode or form black holes as they died. Chandra also developed theories on star atmospheres, black holes, the illumination of the sunlit sky, star structures and star mass. In 1983 Chandra was awarded the Nobel Prize in Physics for his work on the physical processes involved in the structure and evolution of stars. Chandra published ten books and served as the editor of the prominent Astrophysical Journal for nineteen years. In 1999, four years after his death in August of 1995, NASA launched Chandra, a x-ray observatory named in honor of Subrahmanyan Chandrasekhar. The observatory studies the universe in the x-ray portion of the electromagnetic spectrum.<br /> <br /> [[File:Chandra.jpg|200px|thumb|left|alt text]] <br /> <br /> <br /> == Life and Education ==<br /> <br /> Chandrasekhar was born on 19 October 1910 in Lahore, Punjab, India in a Tamil family. At first he was tutored at home by his parents. Later, he attended Hindu High School in Madras to complete his high school education. Consequently, he attended Presidency College in Madras where he obtained his bachelors degree in physics. During this time, he published his first paper &quot;The Compton Scattering and the New Statistics&quot;. After completing his undergraduate studies, he was awarded a scholarship by the govenrment of India. Using this, he was able to pursue his graduate studies in University of Cambridge, under the guidance of professor R. H. Fowler. <br /> <br /> After receiving a bronze medal for his work on degenerate stars, in the summer of 1933, Chandrasekhar was awarded his PhD degree at Cambridge with a thesis among his four papers on rotating self-gravitating polytropes, and the following October, he was elected to a Prize Fellowship at Trinity College for the period 1933–1937.<br /> <br /> == Publications ==<br /> <br /> Chandrasekhar, S. (1958) [1939]. An Introduction to the Study of Stellar Structure. New York: Dover. ISBN 0-486-60413-6.<br /> <br /> Chandrasekhar, S. (2005) [1942]. Principles of Stellar Dynamics. New York: Dover. ISBN 0-486-44273-X.<br /> <br /> Chandrasekhar, S. (1960) [1950]. Radiative Transfer. New York: Dover. ISBN 0-486-60590-6.<br /> <br /> Chandrasekhar, S. (1975) [1960]. Plasma Physics. Chicago: The University of Chicago Press. ISBN 0-226-10084-7.<br /> <br /> Chandrasekhar, S. (1981) [1961]. Hydrodynamic and Hydromagnetic Stability. New York: Dover. ISBN 0-486-64071-X.<br /> <br /> Chandrasekhar, S. (1987) [1969]. Ellipsoidal Figures of Equilibrium. New York: Dover. ISBN 0-486-65258-0.<br /> <br /> Chandrasekhar, S. (1998) [1983]. The Mathematical Theory of Black Holes. New York: Oxford University Press. ISBN 0-19-850370-9.<br /> <br /> Chandrasekhar, S. (1990) [1987]. Truth and Beauty. Aesthetics and Motivations in Science. Chicago: The University of Chicago Press. ISBN 0-226-10087-1.<br /> <br /> Chandrasekhar, S. (1995). Newton's Principia for the Common Reader. Oxford: Clarendon Press. ISBN 0-19-851744-0.<br /> <br /> <br /> == Nobel Prize ==<br /> <br /> The Nobel Prize in Physics 1983 was divided equally between Subramanyan Chandrasekhar &quot;for his theoretical studies of the physical processes of importance to the structure and evolution of the stars&quot; and William Alfred Fowler &quot;for his theoretical and experimental studies of the nuclear reactions of importance in the formation of the chemical elements in the universe&quot;.<br /> <br /> <br /> == Chandrasekhar limit ==<br /> <br /> This was considered to be his greatest contribution to the world of physics. It is based on theories of black holes and dwarf stars. It is important to the field of astrophysics.<br /> <br /> Using Albert Einstein’s special theory of relativity and the principles of quantum physics, Chandrasekhar showed that it is impossible for a white dwarf star, which is supported solely by a degenerate gas of electrons, to be stable if its mass is greater than 1.44 times the mass of the Sun. If such a star does not completely exhaust its thermonuclear fuel, then this limiting mass may be slightly larger.<br /> <br /> All direct mass determinations of actual white dwarf stars have resulted in masses less than the Chandrasekhar limit. A star that ends its nuclear-burning lifetime with a mass greater than the Chandrasekhar limit must become either a neutron star or a black hole.<br /> <br /> [[File:Chandralimit.jpg|200px|thumb|left|alt text]] <br /> <br /> <br /> == References ==<br /> <br /> https://en.wikipedia.org/wiki/Subrahmanyan_Chandrasekhar<br /> http://starchild.gsfc.nasa.gov/docs/StarChild/whos_who_level2/chandra.html</div>

Edcunha3 http://www.physicsbook.gatech.edu/index.php?title=Subrahmanyan_Chandrasekhar&diff=17992 2015-12-06T01:36:05Z

<p>Edcunha3: </p> <hr /> <div>Claimed by Ethan DCunha edcunha3<br /> <br /> Subrahmanyan Chandrasekhar was an Indian American astrophysicist born in Lahore, Punjab. Chandrasekhar was awarded, along with William A. Fowler, the 1983 Nobel Prize for Physics, with Chandrasekhar cited for his mathematical theory of the physical processes of importance to the structure and evolution of the stars. This work led to the currently accepted theory on the later evolutionary stages of massive stars, including black holes.<br /> <br /> Subrahmanyan Chandrasekhar was one of the foremost astrophysicists of the twentieth century. He was one of the first scientists to couple the study of physics with the study of astronomy. Chandra proved that there was an upper limit to the mass of a white dwarf. This limit, known as the Chandra limit, showed that stars more massive than the Sun would explode or form black holes as they died. Chandra also developed theories on star atmospheres, black holes, the illumination of the sunlit sky, star structures and star mass. In 1983 Chandra was awarded the Nobel Prize in Physics for his work on the physical processes involved in the structure and evolution of stars. Chandra published ten books and served as the editor of the prominent Astrophysical Journal for nineteen years. In 1999, four years after his death in August of 1995, NASA launched Chandra, a x-ray observatory named in honor of Subrahmanyan Chandrasekhar. The observatory studies the universe in the x-ray portion of the electromagnetic spectrum.<br /> <br /> <br /> == Life and Education ==<br /> <br /> Chandrasekhar was born on 19 October 1910 in Lahore, Punjab, India in a Tamil family. At first he was tutored at home by his parents. Later, he attended Hindu High School in Madras to complete his high school education. Consequently, he attended Presidency College in Madras where he obtained his bachelors degree in physics. During this time, he published his first paper &quot;The Compton Scattering and the New Statistics&quot;. After completing his undergraduate studies, he was awarded a scholarship by the govenrment of India. Using this, he was able to pursue his graduate studies in University of Cambridge, under the guidance of professor R. H. Fowler. <br /> <br /> After receiving a bronze medal for his work on degenerate stars, in the summer of 1933, Chandrasekhar was awarded his PhD degree at Cambridge with a thesis among his four papers on rotating self-gravitating polytropes, and the following October, he was elected to a Prize Fellowship at Trinity College for the period 1933–1937.<br /> <br /> == Publications ==<br /> <br /> Chandrasekhar, S. (1958) [1939]. An Introduction to the Study of Stellar Structure. New York: Dover. ISBN 0-486-60413-6.<br /> <br /> Chandrasekhar, S. (2005) [1942]. Principles of Stellar Dynamics. New York: Dover. ISBN 0-486-44273-X.<br /> <br /> Chandrasekhar, S. (1960) [1950]. Radiative Transfer. New York: Dover. ISBN 0-486-60590-6.<br /> <br /> Chandrasekhar, S. (1975) [1960]. Plasma Physics. Chicago: The University of Chicago Press. ISBN 0-226-10084-7.<br /> <br /> Chandrasekhar, S. (1981) [1961]. Hydrodynamic and Hydromagnetic Stability. New York: Dover. ISBN 0-486-64071-X.<br /> <br /> Chandrasekhar, S. (1987) [1969]. Ellipsoidal Figures of Equilibrium. New York: Dover. ISBN 0-486-65258-0.<br /> <br /> Chandrasekhar, S. (1998) [1983]. The Mathematical Theory of Black Holes. New York: Oxford University Press. ISBN 0-19-850370-9.<br /> <br /> Chandrasekhar, S. (1990) [1987]. Truth and Beauty. Aesthetics and Motivations in Science. Chicago: The University of Chicago Press. ISBN 0-226-10087-1.<br /> <br /> Chandrasekhar, S. (1995). Newton's Principia for the Common Reader. Oxford: Clarendon Press. ISBN 0-19-851744-0.<br /> <br /> <br /> == Nobel Prize ==<br /> <br /> The Nobel Prize in Physics 1983 was divided equally between Subramanyan Chandrasekhar &quot;for his theoretical studies of the physical processes of importance to the structure and evolution of the stars&quot; and William Alfred Fowler &quot;for his theoretical and experimental studies of the nuclear reactions of importance in the formation of the chemical elements in the universe&quot;.<br /> <br /> <br /> == Chandrasekhar limit ==<br /> <br /> This was considered to be his greatest contribution to the world of physics. It is based on theories of black holes and dwarf stars. It is important to the field of astrophysics.<br /> <br /> Using Albert Einstein’s special theory of relativity and the principles of quantum physics, Chandrasekhar showed that it is impossible for a white dwarf star, which is supported solely by a degenerate gas of electrons, to be stable if its mass is greater than 1.44 times the mass of the Sun. If such a star does not completely exhaust its thermonuclear fuel, then this limiting mass may be slightly larger.<br /> <br /> All direct mass determinations of actual white dwarf stars have resulted in masses less than the Chandrasekhar limit. A star that ends its nuclear-burning lifetime with a mass greater than the Chandrasekhar limit must become either a neutron star or a black hole.<br /> <br /> [[File:Chandralimit.jpg|200px|thumb|left|alt text]] <br /> <br /> <br /> == References ==<br /> <br /> https://en.wikipedia.org/wiki/Subrahmanyan_Chandrasekhar<br /> http://starchild.gsfc.nasa.gov/docs/StarChild/whos_who_level2/chandra.html</div>

Edcunha3 http://www.physicsbook.gatech.edu/index.php?title=File:Chandralimit.jpg&diff=17980 2015-12-06T01:34:50Z

<p>Edcunha3: </p> <hr /> <div></div>

Edcunha3 http://www.physicsbook.gatech.edu/index.php?title=File:Chandu.jpg&diff=17966 2015-12-06T01:32:32Z

<p>Edcunha3: </p> <hr /> <div></div>

Edcunha3 http://www.physicsbook.gatech.edu/index.php?title=Subrahmanyan_Chandrasekhar&diff=16124 2015-12-05T22:17:08Z

<p>Edcunha3: </p> <hr /> <div>Claimed by Ethan DCunha edcunha3<br /> <br /> Subrahmanyan Chandrasekhar was an Indian American astrophysicist born in Lahore, Punjab. Chandrasekhar was awarded, along with William A. Fowler, the 1983 Nobel Prize for Physics, with Chandrasekhar cited for his mathematical theory of the physical processes of importance to the structure and evolution of the stars. This work led to the currently accepted theory on the later evolutionary stages of massive stars, including black holes.<br /> <br /> Subrahmanyan Chandrasekhar was one of the foremost astrophysicists of the twentieth century. He was one of the first scientists to couple the study of physics with the study of astronomy. Chandra proved that there was an upper limit to the mass of a white dwarf. This limit, known as the Chandra limit, showed that stars more massive than the Sun would explode or form black holes as they died. Chandra also developed theories on star atmospheres, black holes, the illumination of the sunlit sky, star structures and star mass. In 1983 Chandra was awarded the Nobel Prize in Physics for his work on the physical processes involved in the structure and evolution of stars. Chandra published ten books and served as the editor of the prominent Astrophysical Journal for nineteen years. In 1999, four years after his death in August of 1995, NASA launched Chandra, a x-ray observatory named in honor of Subrahmanyan Chandrasekhar. The observatory studies the universe in the x-ray portion of the electromagnetic spectrum.<br /> <br /> <br /> == Life and Education ==<br /> <br /> Chandrasekhar was born on 19 October 1910 in Lahore, Punjab, India in a Tamil family. At first he was tutored at home by his parents. Later, he attended Hindu High School in Madras to complete his high school education. Consequently, he attended Presidency College in Madras where he obtained his bachelors degree in physics. During this time, he published his first paper &quot;The Compton Scattering and the New Statistics&quot;. After completing his undergraduate studies, he was awarded a scholarship by the govenrment of India. Using this, he was able to pursue his graduate studies in University of Cambridge, under the guidance of professor R. H. Fowler. <br /> <br /> After receiving a bronze medal for his work on degenerate stars, in the summer of 1933, Chandrasekhar was awarded his PhD degree at Cambridge with a thesis among his four papers on rotating self-gravitating polytropes, and the following October, he was elected to a Prize Fellowship at Trinity College for the period 1933–1937.<br /> <br /> == Publications ==<br /> <br /> Chandrasekhar, S. (1958) [1939]. An Introduction to the Study of Stellar Structure. New York: Dover. ISBN 0-486-60413-6.<br /> <br /> Chandrasekhar, S. (2005) [1942]. Principles of Stellar Dynamics. New York: Dover. ISBN 0-486-44273-X.<br /> <br /> Chandrasekhar, S. (1960) [1950]. Radiative Transfer. New York: Dover. ISBN 0-486-60590-6.<br /> <br /> Chandrasekhar, S. (1975) [1960]. Plasma Physics. Chicago: The University of Chicago Press. ISBN 0-226-10084-7.<br /> <br /> Chandrasekhar, S. (1981) [1961]. Hydrodynamic and Hydromagnetic Stability. New York: Dover. ISBN 0-486-64071-X.<br /> <br /> Chandrasekhar, S. (1987) [1969]. Ellipsoidal Figures of Equilibrium. New York: Dover. ISBN 0-486-65258-0.<br /> <br /> Chandrasekhar, S. (1998) [1983]. The Mathematical Theory of Black Holes. New York: Oxford University Press. ISBN 0-19-850370-9.<br /> <br /> Chandrasekhar, S. (1990) [1987]. Truth and Beauty. Aesthetics and Motivations in Science. Chicago: The University of Chicago Press. ISBN 0-226-10087-1.<br /> <br /> Chandrasekhar, S. (1995). Newton's Principia for the Common Reader. Oxford: Clarendon Press. ISBN 0-19-851744-0.<br /> <br /> <br /> == Nobel Prize ==<br /> <br /> The Nobel Prize in Physics 1983 was divided equally between Subramanyan Chandrasekhar &quot;for his theoretical studies of the physical processes of importance to the structure and evolution of the stars&quot; and William Alfred Fowler &quot;for his theoretical and experimental studies of the nuclear reactions of importance in the formation of the chemical elements in the universe&quot;.<br /> <br /> <br /> == Chandrasekhar limit ==<br /> <br /> This was considered to be his greatest contribution to the world of physics. It is based on theories of black holes and dwarf stars. It is important to the field of astrophysics.<br /> <br /> Using Albert Einstein’s special theory of relativity and the principles of quantum physics, Chandrasekhar showed that it is impossible for a white dwarf star, which is supported solely by a degenerate gas of electrons, to be stable if its mass is greater than 1.44 times the mass of the Sun. If such a star does not completely exhaust its thermonuclear fuel, then this limiting mass may be slightly larger.<br /> <br /> All direct mass determinations of actual white dwarf stars have resulted in masses less than the Chandrasekhar limit. A star that ends its nuclear-burning lifetime with a mass greater than the Chandrasekhar limit must become either a neutron star or a black hole.<br /> <br /> <br /> == References ==<br /> <br /> https://en.wikipedia.org/wiki/Subrahmanyan_Chandrasekhar<br /> http://starchild.gsfc.nasa.gov/docs/StarChild/whos_who_level2/chandra.html</div>

Edcunha3 http://www.physicsbook.gatech.edu/index.php?title=Subrahmanyan_Chandrasekhar&diff=16114 2015-12-05T22:16:18Z

<p>Edcunha3: </p> <hr /> <div>Claimed by Ethan DCunha edcunha3<br /> <br /> Subrahmanyan Chandrasekhar was an Indian American astrophysicist born in Lahore, Punjab. Chandrasekhar was awarded, along with William A. Fowler, the 1983 Nobel Prize for Physics, with Chandrasekhar cited for his mathematical theory of the physical processes of importance to the structure and evolution of the stars. This work led to the currently accepted theory on the later evolutionary stages of massive stars, including black holes.<br /> <br /> Subrahmanyan Chandrasekhar was one of the foremost astrophysicists of the twentieth century. He was one of the first scientists to couple the study of physics with the study of astronomy. Chandra proved that there was an upper limit to the mass of a white dwarf. This limit, known as the Chandra limit, showed that stars more massive than the Sun would explode or form black holes as they died. Chandra also developed theories on star atmospheres, black holes, the illumination of the sunlit sky, star structures and star mass. In 1983 Chandra was awarded the Nobel Prize in Physics for his work on the physical processes involved in the structure and evolution of stars. Chandra published ten books and served as the editor of the prominent Astrophysical Journal for nineteen years. In 1999, four years after his death in August of 1995, NASA launched Chandra, a x-ray observatory named in honor of Subrahmanyan Chandrasekhar. The observatory studies the universe in the x-ray portion of the electromagnetic spectrum.<br /> <br /> [[File:http://th.physik.uni-frankfurt.de/~jr/gif/phys/chandra.jpg]]<br /> <br /> == Life and Education ==<br /> <br /> Chandrasekhar was born on 19 October 1910 in Lahore, Punjab, India in a Tamil family. At first he was tutored at home by his parents. Later, he attended Hindu High School in Madras to complete his high school education. Consequently, he attended Presidency College in Madras where he obtained his bachelors degree in physics. During this time, he published his first paper &quot;The Compton Scattering and the New Statistics&quot;. After completing his undergraduate studies, he was awarded a scholarship by the govenrment of India. Using this, he was able to pursue his graduate studies in University of Cambridge, under the guidance of professor R. H. Fowler. <br /> <br /> After receiving a bronze medal for his work on degenerate stars, in the summer of 1933, Chandrasekhar was awarded his PhD degree at Cambridge with a thesis among his four papers on rotating self-gravitating polytropes, and the following October, he was elected to a Prize Fellowship at Trinity College for the period 1933–1937.<br /> <br /> == Publications ==<br /> <br /> Chandrasekhar, S. (1958) [1939]. An Introduction to the Study of Stellar Structure. New York: Dover. ISBN 0-486-60413-6.<br /> <br /> Chandrasekhar, S. (2005) [1942]. Principles of Stellar Dynamics. New York: Dover. ISBN 0-486-44273-X.<br /> <br /> Chandrasekhar, S. (1960) [1950]. Radiative Transfer. New York: Dover. ISBN 0-486-60590-6.<br /> <br /> Chandrasekhar, S. (1975) [1960]. Plasma Physics. Chicago: The University of Chicago Press. ISBN 0-226-10084-7.<br /> <br /> Chandrasekhar, S. (1981) [1961]. Hydrodynamic and Hydromagnetic Stability. New York: Dover. ISBN 0-486-64071-X.<br /> <br /> Chandrasekhar, S. (1987) [1969]. Ellipsoidal Figures of Equilibrium. New York: Dover. ISBN 0-486-65258-0.<br /> <br /> Chandrasekhar, S. (1998) [1983]. The Mathematical Theory of Black Holes. New York: Oxford University Press. ISBN 0-19-850370-9.<br /> <br /> Chandrasekhar, S. (1990) [1987]. Truth and Beauty. Aesthetics and Motivations in Science. Chicago: The University of Chicago Press. ISBN 0-226-10087-1.<br /> <br /> Chandrasekhar, S. (1995). Newton's Principia for the Common Reader. Oxford: Clarendon Press. ISBN 0-19-851744-0.<br /> <br /> <br /> == Nobel Prize ==<br /> <br /> The Nobel Prize in Physics 1983 was divided equally between Subramanyan Chandrasekhar &quot;for his theoretical studies of the physical processes of importance to the structure and evolution of the stars&quot; and William Alfred Fowler &quot;for his theoretical and experimental studies of the nuclear reactions of importance in the formation of the chemical elements in the universe&quot;.<br /> <br /> <br /> == Chandrasekhar limit ==<br /> <br /> This was considered to be his greatest contribution to the world of physics. It is based on theories of black holes and dwarf stars. It is important to the field of astrophysics.<br /> <br /> Using Albert Einstein’s special theory of relativity and the principles of quantum physics, Chandrasekhar showed that it is impossible for a white dwarf star, which is supported solely by a degenerate gas of electrons, to be stable if its mass is greater than 1.44 times the mass of the Sun. If such a star does not completely exhaust its thermonuclear fuel, then this limiting mass may be slightly larger.<br /> <br /> All direct mass determinations of actual white dwarf stars have resulted in masses less than the Chandrasekhar limit. A star that ends its nuclear-burning lifetime with a mass greater than the Chandrasekhar limit must become either a neutron star or a black hole.<br /> <br /> <br /> == References ==<br /> <br /> https://en.wikipedia.org/wiki/Subrahmanyan_Chandrasekhar<br /> http://starchild.gsfc.nasa.gov/docs/StarChild/whos_who_level2/chandra.html</div>

Edcunha3 http://www.physicsbook.gatech.edu/index.php?title=Subrahmanyan_Chandrasekhar&diff=12811 2015-12-04T23:05:36Z

<p>Edcunha3: </p> <hr /> <div>Claimed by Ethan DCunha edcunha3<br /> <br /> Subrahmanyan Chandrasekhar was an Indian American astrophysicist born in Lahore, Punjab. Chandrasekhar was awarded, along with William A. Fowler, the 1983 Nobel Prize for Physics, with Chandrasekhar cited for his mathematical theory of the physical processes of importance to the structure and evolution of the stars. This work led to the currently accepted theory on the later evolutionary stages of massive stars, including black holes.<br /> <br /> Subrahmanyan Chandrasekhar was one of the foremost astrophysicists of the twentieth century. He was one of the first scientists to couple the study of physics with the study of astronomy. Chandra proved that there was an upper limit to the mass of a white dwarf. This limit, known as the Chandra limit, showed that stars more massive than the Sun would explode or form black holes as they died. Chandra also developed theories on star atmospheres, black holes, the illumination of the sunlit sky, star structures and star mass. In 1983 Chandra was awarded the Nobel Prize in Physics for his work on the physical processes involved in the structure and evolution of stars. Chandra published ten books and served as the editor of the prominent Astrophysical Journal for nineteen years. In 1999, four years after his death in August of 1995, NASA launched Chandra, a x-ray observatory named in honor of Subrahmanyan Chandrasekhar. The observatory studies the universe in the x-ray portion of the electromagnetic spectrum.<br /> <br /> <br /> == Life and Education ==<br /> <br /> Chandrasekhar was born on 19 October 1910 in Lahore, Punjab, India in a Tamil family. At first he was tutored at home by his parents. Later, he attended Hindu High School in Madras to complete his high school education. Consequently, he attended Presidency College in Madras where he obtained his bachelors degree in physics. During this time, he published his first paper &quot;The Compton Scattering and the New Statistics&quot;. After completing his undergraduate studies, he was awarded a scholarship by the govenrment of India. Using this, he was able to pursue his graduate studies in University of Cambridge, under the guidance of professor R. H. Fowler. <br /> <br /> After receiving a bronze medal for his work on degenerate stars, in the summer of 1933, Chandrasekhar was awarded his PhD degree at Cambridge with a thesis among his four papers on rotating self-gravitating polytropes, and the following October, he was elected to a Prize Fellowship at Trinity College for the period 1933–1937.<br /> <br /> == Publications ==<br /> <br /> Chandrasekhar, S. (1958) [1939]. An Introduction to the Study of Stellar Structure. New York: Dover. ISBN 0-486-60413-6.<br /> <br /> Chandrasekhar, S. (2005) [1942]. Principles of Stellar Dynamics. New York: Dover. ISBN 0-486-44273-X.<br /> <br /> Chandrasekhar, S. (1960) [1950]. Radiative Transfer. New York: Dover. ISBN 0-486-60590-6.<br /> <br /> Chandrasekhar, S. (1975) [1960]. Plasma Physics. Chicago: The University of Chicago Press. ISBN 0-226-10084-7.<br /> <br /> Chandrasekhar, S. (1981) [1961]. Hydrodynamic and Hydromagnetic Stability. New York: Dover. ISBN 0-486-64071-X.<br /> <br /> Chandrasekhar, S. (1987) [1969]. Ellipsoidal Figures of Equilibrium. New York: Dover. ISBN 0-486-65258-0.<br /> <br /> Chandrasekhar, S. (1998) [1983]. The Mathematical Theory of Black Holes. New York: Oxford University Press. ISBN 0-19-850370-9.<br /> <br /> Chandrasekhar, S. (1990) [1987]. Truth and Beauty. Aesthetics and Motivations in Science. Chicago: The University of Chicago Press. ISBN 0-226-10087-1.<br /> <br /> Chandrasekhar, S. (1995). Newton's Principia for the Common Reader. Oxford: Clarendon Press. ISBN 0-19-851744-0.<br /> <br /> <br /> == Nobel Prize ==<br /> <br /> The Nobel Prize in Physics 1983 was divided equally between Subramanyan Chandrasekhar &quot;for his theoretical studies of the physical processes of importance to the structure and evolution of the stars&quot; and William Alfred Fowler &quot;for his theoretical and experimental studies of the nuclear reactions of importance in the formation of the chemical elements in the universe&quot;.<br /> <br /> <br /> == Chandrasekhar limit ==<br /> <br /> This was considered to be his greatest contribution to the world of physics. It is based on theories of black holes and dwarf stars. It is important to the field of astrophysics.<br /> <br /> Using Albert Einstein’s special theory of relativity and the principles of quantum physics, Chandrasekhar showed that it is impossible for a white dwarf star, which is supported solely by a degenerate gas of electrons, to be stable if its mass is greater than 1.44 times the mass of the Sun. If such a star does not completely exhaust its thermonuclear fuel, then this limiting mass may be slightly larger.<br /> <br /> All direct mass determinations of actual white dwarf stars have resulted in masses less than the Chandrasekhar limit. A star that ends its nuclear-burning lifetime with a mass greater than the Chandrasekhar limit must become either a neutron star or a black hole.<br /> <br /> <br /> == References ==<br /> <br /> https://en.wikipedia.org/wiki/Subrahmanyan_Chandrasekhar<br /> http://starchild.gsfc.nasa.gov/docs/StarChild/whos_who_level2/chandra.html</div>

Edcunha3 http://www.physicsbook.gatech.edu/index.php?title=Subrahmanyan_Chandrasekhar&diff=12804 2015-12-04T22:53:50Z

<p>Edcunha3: </p> <hr /> <div>Claimed by Ethan DCunha edcunha3<br /> <br /> Subrahmanyan Chandrasekhar was an Indian American astrophysicist born in Lahore, Punjab. Chandrasekhar was awarded, along with William A. Fowler, the 1983 Nobel Prize for Physics, with Chandrasekhar cited for his mathematical theory of the physical processes of importance to the structure and evolution of the stars. This work led to the currently accepted theory on the later evolutionary stages of massive stars, including black holes.<br /> <br /> Subrahmanyan Chandrasekhar was one of the foremost astrophysicists of the twentieth century. He was one of the first scientists to couple the study of physics with the study of astronomy. Chandra proved that there was an upper limit to the mass of a white dwarf. This limit, known as the Chandra limit, showed that stars more massive than the Sun would explode or form black holes as they died. Chandra also developed theories on star atmospheres, black holes, the illumination of the sunlit sky, star structures and star mass. In 1983 Chandra was awarded the Nobel Prize in Physics for his work on the physical processes involved in the structure and evolution of stars. Chandra published ten books and served as the editor of the prominent Astrophysical Journal for nineteen years. In 1999, four years after his death in August of 1995, NASA launched Chandra, a x-ray observatory named in honor of Subrahmanyan Chandrasekhar. The observatory studies the universe in the x-ray portion of the electromagnetic spectrum.<br /> <br /> <br /> == Life and Education ==<br /> <br /> Chandrasekhar was born on 19 October 1910 in Lahore, Punjab, India in a Tamil family. At first he was tutored at home by his parents. Later, he attended Hindu High School in Madras to complete his high school education. Consequently, he attended Presidency College in Madras where he obtained his bachelors degree in physics. During this time, he published his first paper &quot;The Compton Scattering and the New Statistics&quot;. After completing his undergraduate studies, he was awarded a scholarship by the govenrment of India. Using this, he was able to pursue his graduate studies in University of Cambridge, under the guidance of professor R. H. Fowler. <br /> <br /> After receiving a bronze medal for his work on degenerate stars, in the summer of 1933, Chandrasekhar was awarded his PhD degree at Cambridge with a thesis among his four papers on rotating self-gravitating polytropes, and the following October, he was elected to a Prize Fellowship at Trinity College for the period 1933–1937.<br /> <br /> == Publications ==<br /> <br /> Chandrasekhar, S. (1958) [1939]. An Introduction to the Study of Stellar Structure. New York: Dover. ISBN 0-486-60413-6.<br /> <br /> Chandrasekhar, S. (2005) [1942]. Principles of Stellar Dynamics. New York: Dover. ISBN 0-486-44273-X.<br /> <br /> Chandrasekhar, S. (1960) [1950]. Radiative Transfer. New York: Dover. ISBN 0-486-60590-6.<br /> <br /> Chandrasekhar, S. (1975) [1960]. Plasma Physics. Chicago: The University of Chicago Press. ISBN 0-226-10084-7.<br /> <br /> Chandrasekhar, S. (1981) [1961]. Hydrodynamic and Hydromagnetic Stability. New York: Dover. ISBN 0-486-64071-X.<br /> <br /> Chandrasekhar, S. (1987) [1969]. Ellipsoidal Figures of Equilibrium. New York: Dover. ISBN 0-486-65258-0.<br /> <br /> Chandrasekhar, S. (1998) [1983]. The Mathematical Theory of Black Holes. New York: Oxford University Press. ISBN 0-19-850370-9.<br /> <br /> Chandrasekhar, S. (1990) [1987]. Truth and Beauty. Aesthetics and Motivations in Science. Chicago: The University of Chicago Press. ISBN 0-226-10087-1.<br /> <br /> Chandrasekhar, S. (1995). Newton's Principia for the Common Reader. Oxford: Clarendon Press. ISBN 0-19-851744-0.<br /> <br /> <br /> == Nobel Prize ==<br /> <br /> The Nobel Prize in Physics 1983 was divided equally between Subramanyan Chandrasekhar &quot;for his theoretical studies of the physical processes of importance to the structure and evolution of the stars&quot; and William Alfred Fowler &quot;for his theoretical and experimental studies of the nuclear reactions of importance in the formation of the chemical elements in the universe&quot;.<br /> <br /> <br /> == Chandrasekhar limit ==<br /> <br /> This was considered to be his greatest contribution to the world of physics. It is based on theories of black holes and dwarf stars. It is important to the field of astrophysics.<br /> <br /> Using Albert Einstein’s special theory of relativity and the principles of quantum physics, Chandrasekhar showed that it is impossible for a white dwarf star, which is supported solely by a degenerate gas of electrons, to be stable if its mass is greater than 1.44 times the mass of the Sun. If such a star does not completely exhaust its thermonuclear fuel, then this limiting mass may be slightly larger.<br /> <br /> All direct mass determinations of actual white dwarf stars have resulted in masses less than the Chandrasekhar limit. A star that ends its nuclear-burning lifetime with a mass greater than the Chandrasekhar limit must become either a neutron star or a black hole.</div>

Edcunha3 http://www.physicsbook.gatech.edu/index.php?title=Subrahmanyan_Chandrasekhar&diff=12803 2015-12-04T22:52:44Z

<p>Edcunha3: </p> <hr /> <div><br /> <br /> Subrahmanyan Chandrasekhar was an Indian American astrophysicist born in Lahore, Punjab. Chandrasekhar was awarded, along with William A. Fowler, the 1983 Nobel Prize for Physics, with Chandrasekhar cited for his mathematical theory of the physical processes of importance to the structure and evolution of the stars. This work led to the currently accepted theory on the later evolutionary stages of massive stars, including black holes.<br /> <br /> Subrahmanyan Chandrasekhar was one of the foremost astrophysicists of the twentieth century. He was one of the first scientists to couple the study of physics with the study of astronomy. Chandra proved that there was an upper limit to the mass of a white dwarf. This limit, known as the Chandra limit, showed that stars more massive than the Sun would explode or form black holes as they died. Chandra also developed theories on star atmospheres, black holes, the illumination of the sunlit sky, star structures and star mass. In 1983 Chandra was awarded the Nobel Prize in Physics for his work on the physical processes involved in the structure and evolution of stars. Chandra published ten books and served as the editor of the prominent Astrophysical Journal for nineteen years. In 1999, four years after his death in August of 1995, NASA launched Chandra, a x-ray observatory named in honor of Subrahmanyan Chandrasekhar. The observatory studies the universe in the x-ray portion of the electromagnetic spectrum.<br /> <br /> <br /> == Life and Education ==<br /> <br /> Chandrasekhar was born on 19 October 1910 in Lahore, Punjab, India in a Tamil family. At first he was tutored at home by his parents. Later, he attended Hindu High School in Madras to complete his high school education. Consequently, he attended Presidency College in Madras where he obtained his bachelors degree in physics. During this time, he published his first paper &quot;The Compton Scattering and the New Statistics&quot;. After completing his undergraduate studies, he was awarded a scholarship by the govenrment of India. Using this, he was able to pursue his graduate studies in University of Cambridge, under the guidance of professor R. H. Fowler. <br /> <br /> After receiving a bronze medal for his work on degenerate stars, in the summer of 1933, Chandrasekhar was awarded his PhD degree at Cambridge with a thesis among his four papers on rotating self-gravitating polytropes, and the following October, he was elected to a Prize Fellowship at Trinity College for the period 1933–1937.<br /> <br /> == Publications ==<br /> <br /> Chandrasekhar, S. (1958) [1939]. An Introduction to the Study of Stellar Structure. New York: Dover. ISBN 0-486-60413-6.<br /> <br /> Chandrasekhar, S. (2005) [1942]. Principles of Stellar Dynamics. New York: Dover. ISBN 0-486-44273-X.<br /> <br /> Chandrasekhar, S. (1960) [1950]. Radiative Transfer. New York: Dover. ISBN 0-486-60590-6.<br /> <br /> Chandrasekhar, S. (1975) [1960]. Plasma Physics. Chicago: The University of Chicago Press. ISBN 0-226-10084-7.<br /> <br /> Chandrasekhar, S. (1981) [1961]. Hydrodynamic and Hydromagnetic Stability. New York: Dover. ISBN 0-486-64071-X.<br /> <br /> Chandrasekhar, S. (1987) [1969]. Ellipsoidal Figures of Equilibrium. New York: Dover. ISBN 0-486-65258-0.<br /> <br /> Chandrasekhar, S. (1998) [1983]. The Mathematical Theory of Black Holes. New York: Oxford University Press. ISBN 0-19-850370-9.<br /> <br /> Chandrasekhar, S. (1990) [1987]. Truth and Beauty. Aesthetics and Motivations in Science. Chicago: The University of Chicago Press. ISBN 0-226-10087-1.<br /> <br /> Chandrasekhar, S. (1995). Newton's Principia for the Common Reader. Oxford: Clarendon Press. ISBN 0-19-851744-0.<br /> <br /> <br /> == Nobel Prize ==<br /> <br /> The Nobel Prize in Physics 1983 was divided equally between Subramanyan Chandrasekhar &quot;for his theoretical studies of the physical processes of importance to the structure and evolution of the stars&quot; and William Alfred Fowler &quot;for his theoretical and experimental studies of the nuclear reactions of importance in the formation of the chemical elements in the universe&quot;.<br /> <br /> <br /> == Chandrasekhar limit ==<br /> <br /> This was considered to be his greatest contribution to the world of physics. It is based on theories of black holes and dwarf stars. It is important to the field of astrophysics.<br /> <br /> Using Albert Einstein’s special theory of relativity and the principles of quantum physics, Chandrasekhar showed that it is impossible for a white dwarf star, which is supported solely by a degenerate gas of electrons, to be stable if its mass is greater than 1.44 times the mass of the Sun. If such a star does not completely exhaust its thermonuclear fuel, then this limiting mass may be slightly larger.<br /> <br /> All direct mass determinations of actual white dwarf stars have resulted in masses less than the Chandrasekhar limit. A star that ends its nuclear-burning lifetime with a mass greater than the Chandrasekhar limit must become either a neutron star or a black hole.</div>

Edcunha3 http://www.physicsbook.gatech.edu/index.php?title=Subrahmanyan_Chandrasekhar&diff=12801 2015-12-04T22:52:20Z

<p>Edcunha3: </p> <hr /> <div><br /> <br /> Subrahmanyan Chandrasekhar was an Indian American astrophysicist born in Lahore, Punjab. Chandrasekhar was awarded, along with William A. Fowler, the 1983 Nobel Prize for Physics, with Chandrasekhar cited for his mathematical theory of the physical processes of importance to the structure and evolution of the stars. This work led to the currently accepted theory on the later evolutionary stages of massive stars, including black holes.<br /> <br /> Subrahmanyan Chandrasekhar was one of the foremost astrophysicists of the twentieth century. He was one of the first scientists to couple the study of physics with the study of astronomy. Chandra proved that there was an upper limit to the mass of a white dwarf. This limit, known as the Chandra limit, showed that stars more massive than the Sun would explode or form black holes as they died. Chandra also developed theories on star atmospheres, black holes, the illumination of the sunlit sky, star structures and star mass. In 1983 Chandra was awarded the Nobel Prize in Physics for his work on the physical processes involved in the structure and evolution of stars. Chandra published ten books and served as the editor of the prominent Astrophysical Journal for nineteen years. In 1999, four years after his death in August of 1995, NASA launched Chandra, a x-ray observatory named in honor of Subrahmanyan Chandrasekhar. The observatory studies the universe in the x-ray portion of the electromagnetic spectrum.<br /> [[C:\Users\Ethan\Desktop:Chandu.jpg]]<br /> <br /> == Life and Education ==<br /> <br /> Chandrasekhar was born on 19 October 1910 in Lahore, Punjab, India in a Tamil family. At first he was tutored at home by his parents. Later, he attended Hindu High School in Madras to complete his high school education. Consequently, he attended Presidency College in Madras where he obtained his bachelors degree in physics. During this time, he published his first paper &quot;The Compton Scattering and the New Statistics&quot;. After completing his undergraduate studies, he was awarded a scholarship by the govenrment of India. Using this, he was able to pursue his graduate studies in University of Cambridge, under the guidance of professor R. H. Fowler. <br /> <br /> After receiving a bronze medal for his work on degenerate stars, in the summer of 1933, Chandrasekhar was awarded his PhD degree at Cambridge with a thesis among his four papers on rotating self-gravitating polytropes, and the following October, he was elected to a Prize Fellowship at Trinity College for the period 1933–1937.<br /> <br /> == Publications ==<br /> <br /> Chandrasekhar, S. (1958) [1939]. An Introduction to the Study of Stellar Structure. New York: Dover. ISBN 0-486-60413-6.<br /> <br /> Chandrasekhar, S. (2005) [1942]. Principles of Stellar Dynamics. New York: Dover. ISBN 0-486-44273-X.<br /> <br /> Chandrasekhar, S. (1960) [1950]. Radiative Transfer. New York: Dover. ISBN 0-486-60590-6.<br /> <br /> Chandrasekhar, S. (1975) [1960]. Plasma Physics. Chicago: The University of Chicago Press. ISBN 0-226-10084-7.<br /> <br /> Chandrasekhar, S. (1981) [1961]. Hydrodynamic and Hydromagnetic Stability. New York: Dover. ISBN 0-486-64071-X.<br /> <br /> Chandrasekhar, S. (1987) [1969]. Ellipsoidal Figures of Equilibrium. New York: Dover. ISBN 0-486-65258-0.<br /> <br /> Chandrasekhar, S. (1998) [1983]. The Mathematical Theory of Black Holes. New York: Oxford University Press. ISBN 0-19-850370-9.<br /> <br /> Chandrasekhar, S. (1990) [1987]. Truth and Beauty. Aesthetics and Motivations in Science. Chicago: The University of Chicago Press. ISBN 0-226-10087-1.<br /> <br /> Chandrasekhar, S. (1995). Newton's Principia for the Common Reader. Oxford: Clarendon Press. ISBN 0-19-851744-0.<br /> <br /> <br /> == Nobel Prize ==<br /> <br /> The Nobel Prize in Physics 1983 was divided equally between Subramanyan Chandrasekhar &quot;for his theoretical studies of the physical processes of importance to the structure and evolution of the stars&quot; and William Alfred Fowler &quot;for his theoretical and experimental studies of the nuclear reactions of importance in the formation of the chemical elements in the universe&quot;.<br /> <br /> <br /> == Chandrasekhar limit ==<br /> <br /> This was considered to be his greatest contribution to the world of physics. It is based on theories of black holes and dwarf stars. It is important to the field of astrophysics.<br /> <br /> Using Albert Einstein’s special theory of relativity and the principles of quantum physics, Chandrasekhar showed that it is impossible for a white dwarf star, which is supported solely by a degenerate gas of electrons, to be stable if its mass is greater than 1.44 times the mass of the Sun. If such a star does not completely exhaust its thermonuclear fuel, then this limiting mass may be slightly larger.<br /> <br /> All direct mass determinations of actual white dwarf stars have resulted in masses less than the Chandrasekhar limit. A star that ends its nuclear-burning lifetime with a mass greater than the Chandrasekhar limit must become either a neutron star or a black hole.</div>

Edcunha3 http://www.physicsbook.gatech.edu/index.php?title=Subrahmanyan_Chandrasekhar&diff=12797 2015-12-04T22:50:05Z

<p>Edcunha3: </p> <hr /> <div><br /> <br /> Subrahmanyan Chandrasekhar was an Indian American astrophysicist born in Lahore, Punjab. Chandrasekhar was awarded, along with William A. Fowler, the 1983 Nobel Prize for Physics, with Chandrasekhar cited for his mathematical theory of the physical processes of importance to the structure and evolution of the stars. This work led to the currently accepted theory on the later evolutionary stages of massive stars, including black holes.<br /> <br /> Subrahmanyan Chandrasekhar was one of the foremost astrophysicists of the twentieth century. He was one of the first scientists to couple the study of physics with the study of astronomy. Chandra proved that there was an upper limit to the mass of a white dwarf. This limit, known as the Chandra limit, showed that stars more massive than the Sun would explode or form black holes as they died. Chandra also developed theories on star atmospheres, black holes, the illumination of the sunlit sky, star structures and star mass. In 1983 Chandra was awarded the Nobel Prize in Physics for his work on the physical processes involved in the structure and evolution of stars. Chandra published ten books and served as the editor of the prominent Astrophysical Journal for nineteen years. In 1999, four years after his death in August of 1995, NASA launched Chandra, a x-ray observatory named in honor of Subrahmanyan Chandrasekhar. The observatory studies the universe in the x-ray portion of the electromagnetic spectrum.<br /> <br /> <br /> == Life and Education ==<br /> <br /> Chandrasekhar was born on 19 October 1910 in Lahore, Punjab, India in a Tamil family. At first he was tutored at home by his parents. Later, he attended Hindu High School in Madras to complete his high school education. Consequently, he attended Presidency College in Madras where he obtained his bachelors degree in physics. During this time, he published his first paper &quot;The Compton Scattering and the New Statistics&quot;. After completing his undergraduate studies, he was awarded a scholarship by the govenrment of India. Using this, he was able to pursue his graduate studies in University of Cambridge, under the guidance of professor R. H. Fowler. <br /> <br /> After receiving a bronze medal for his work on degenerate stars, in the summer of 1933, Chandrasekhar was awarded his PhD degree at Cambridge with a thesis among his four papers on rotating self-gravitating polytropes, and the following October, he was elected to a Prize Fellowship at Trinity College for the period 1933–1937.<br /> <br /> == Publications ==<br /> <br /> Chandrasekhar, S. (1958) [1939]. An Introduction to the Study of Stellar Structure. New York: Dover. ISBN 0-486-60413-6.<br /> <br /> Chandrasekhar, S. (2005) [1942]. Principles of Stellar Dynamics. New York: Dover. ISBN 0-486-44273-X.<br /> <br /> Chandrasekhar, S. (1960) [1950]. Radiative Transfer. New York: Dover. ISBN 0-486-60590-6.<br /> <br /> Chandrasekhar, S. (1975) [1960]. Plasma Physics. Chicago: The University of Chicago Press. ISBN 0-226-10084-7.<br /> <br /> Chandrasekhar, S. (1981) [1961]. Hydrodynamic and Hydromagnetic Stability. New York: Dover. ISBN 0-486-64071-X.<br /> <br /> Chandrasekhar, S. (1987) [1969]. Ellipsoidal Figures of Equilibrium. New York: Dover. ISBN 0-486-65258-0.<br /> <br /> Chandrasekhar, S. (1998) [1983]. The Mathematical Theory of Black Holes. New York: Oxford University Press. ISBN 0-19-850370-9.<br /> <br /> Chandrasekhar, S. (1990) [1987]. Truth and Beauty. Aesthetics and Motivations in Science. Chicago: The University of Chicago Press. ISBN 0-226-10087-1.<br /> <br /> Chandrasekhar, S. (1995). Newton's Principia for the Common Reader. Oxford: Clarendon Press. ISBN 0-19-851744-0.<br /> <br /> <br /> == Nobel Prize ==<br /> <br /> The Nobel Prize in Physics 1983 was divided equally between Subramanyan Chandrasekhar &quot;for his theoretical studies of the physical processes of importance to the structure and evolution of the stars&quot; and William Alfred Fowler &quot;for his theoretical and experimental studies of the nuclear reactions of importance in the formation of the chemical elements in the universe&quot;.<br /> <br /> <br /> == Chandrasekhar limit ==<br /> <br /> This was considered to be his greatest contribution to the world of physics. It is based on theories of black holes and dwarf stars. It is important to the field of astrophysics.<br /> <br /> Using Albert Einstein’s special theory of relativity and the principles of quantum physics, Chandrasekhar showed that it is impossible for a white dwarf star, which is supported solely by a degenerate gas of electrons, to be stable if its mass is greater than 1.44 times the mass of the Sun. If such a star does not completely exhaust its thermonuclear fuel, then this limiting mass may be slightly larger.<br /> <br /> All direct mass determinations of actual white dwarf stars have resulted in masses less than the Chandrasekhar limit. A star that ends its nuclear-burning lifetime with a mass greater than the Chandrasekhar limit must become either a neutron star or a black hole.</div>

Edcunha3 http://www.physicsbook.gatech.edu/index.php?title=Subrahmanyan_Chandrasekhar&diff=12789 2015-12-04T22:44:05Z

<p>Edcunha3: </p> <hr /> <div><br /> <br /> Subrahmanyan Chandrasekhar was an Indian American astrophysicist born in Lahore, Punjab. Chandrasekhar was awarded, along with William A. Fowler, the 1983 Nobel Prize for Physics, with Chandrasekhar cited for his mathematical theory of the physical processes of importance to the structure and evolution of the stars. This work led to the currently accepted theory on the later evolutionary stages of massive stars, including black holes.<br /> <br /> Subrahmanyan Chandrasekhar was one of the foremost astrophysicists of the twentieth century. He was one of the first scientists to couple the study of physics with the study of astronomy. Chandra proved that there was an upper limit to the mass of a white dwarf. This limit, known as the Chandra limit, showed that stars more massive than the Sun would explode or form black holes as they died. Chandra also developed theories on star atmospheres, black holes, the illumination of the sunlit sky, star structures and star mass. In 1983 Chandra was awarded the Nobel Prize in Physics for his work on the physical processes involved in the structure and evolution of stars. Chandra published ten books and served as the editor of the prominent Astrophysical Journal for nineteen years. In 1999, four years after his death in August of 1995, NASA launched Chandra, a x-ray observatory named in honor of Subrahmanyan Chandrasekhar. The observatory studies the universe in the x-ray portion of the electromagnetic spectrum.<br /> <br /> <br /> == Life and Education ==<br /> <br /> Chandrasekhar was born on 19 October 1910 in Lahore, Punjab, India in a Tamil family. At first he was tutored at home by his parents. Later, he attended Hindu High School in Madras to complete his high school education. <br /> == Publications ==<br /> <br /> Chandrasekhar, S. (1958) [1939]. An Introduction to the Study of Stellar Structure. New York: Dover. ISBN 0-486-60413-6.<br /> Chandrasekhar, S. (2005) [1942]. Principles of Stellar Dynamics. New York: Dover. ISBN 0-486-44273-X.<br /> Chandrasekhar, S. (1960) [1950]. Radiative Transfer. New York: Dover. ISBN 0-486-60590-6.<br /> Chandrasekhar, S. (1975) [1960]. Plasma Physics. Chicago: The University of Chicago Press. ISBN 0-226-10084-7.<br /> Chandrasekhar, S. (1981) [1961]. Hydrodynamic and Hydromagnetic Stability. New York: Dover. ISBN 0-486-64071-X.<br /> Chandrasekhar, S. (1987) [1969]. Ellipsoidal Figures of Equilibrium. New York: Dover. ISBN 0-486-65258-0.<br /> Chandrasekhar, S. (1998) [1983]. The Mathematical Theory of Black Holes. New York: Oxford University Press. ISBN 0-19-850370-9.<br /> Chandrasekhar, S. (1990) [1987]. Truth and Beauty. Aesthetics and Motivations in Science. Chicago: The University of Chicago Press. ISBN 0-226-10087-1.<br /> Chandrasekhar, S. (1995). Newton's Principia for the Common Reader. Oxford: Clarendon Press. ISBN 0-19-851744-0.<br /> <br /> <br /> == Nobel Prize ==<br /> <br /> The Nobel Prize in Physics 1983 was divided equally between Subramanyan Chandrasekhar &quot;for his theoretical studies of the physical processes of importance to the structure and evolution of the stars&quot; and William Alfred Fowler &quot;for his theoretical and experimental studies of the nuclear reactions of importance in the formation of the chemical elements in the universe&quot;.<br /> <br /> <br /> == Chandrasekhar limit ==<br /> <br /> This was considered to be his greatest contribution to the world of physics. It is based on theories of black holes and dwarf stars. It is important to the field of astrophysics.<br /> <br /> Using Albert Einstein’s special theory of relativity and the principles of quantum physics, Chandrasekhar showed that it is impossible for a white dwarf star, which is supported solely by a degenerate gas of electrons, to be stable if its mass is greater than 1.44 times the mass of the Sun. If such a star does not completely exhaust its thermonuclear fuel, then this limiting mass may be slightly larger.<br /> <br /> All direct mass determinations of actual white dwarf stars have resulted in masses less than the Chandrasekhar limit. A star that ends its nuclear-burning lifetime with a mass greater than the Chandrasekhar limit must become either a neutron star or a black hole.</div>

Edcunha3 http://www.physicsbook.gatech.edu/index.php?title=Subrahmanyan_Chandrasekhar&diff=12787 2015-12-04T22:43:32Z

<p>Edcunha3: </p> <hr /> <div><br /> <br /> Subrahmanyan Chandrasekhar was an Indian American astrophysicist born in Lahore, Punjab. Chandrasekhar was awarded, along with William A. Fowler, the 1983 Nobel Prize for Physics, with Chandrasekhar cited for his mathematical theory of the physical processes of importance to the structure and evolution of the stars. This work led to the currently accepted theory on the later evolutionary stages of massive stars, including black holes.<br /> <br /> Subrahmanyan Chandrasekhar was one of the foremost astrophysicists of the twentieth century. He was one of the first scientists to couple the study of physics with the study of astronomy. Chandra proved that there was an upper limit to the mass of a white dwarf. This limit, known as the Chandra limit, showed that stars more massive than the Sun would explode or form black holes as they died. Chandra also developed theories on star atmospheres, black holes, the illumination of the sunlit sky, star structures and star mass. In 1983 Chandra was awarded the Nobel Prize in Physics for his work on the physical processes involved in the structure and evolution of stars. Chandra published ten books and served as the editor of the prominent Astrophysical Journal for nineteen years. In 1999, four years after his death in August of 1995, NASA launched Chandra, a x-ray observatory named in honor of Subrahmanyan Chandrasekhar. The observatory studies the universe in the x-ray portion of the electromagnetic spectrum.<br /> <br /> <br /> == Life and Education ==<br /> <br /> Chandrasekhar was born on 19 October 1910 in Lahore, Punjab, India in a Tamil family. At first he was tutored at home by his parents. Later, he attended Hindu High School in Madras to complete his high school education. <br /> == Publications ==<br /> <br /> Chandrasekhar, S. (1958) [1939]. An Introduction to the Study of Stellar Structure. New York: Dover. ISBN 0-486-60413-6.<br /> Chandrasekhar, S. (2005) [1942]. Principles of Stellar Dynamics. New York: Dover. ISBN 0-486-44273-X.<br /> Chandrasekhar, S. (1960) [1950]. Radiative Transfer. New York: Dover. ISBN 0-486-60590-6.<br /> Chandrasekhar, S. (1975) [1960]. Plasma Physics. Chicago: The University of Chicago Press. ISBN 0-226-10084-7.<br /> Chandrasekhar, S. (1981) [1961]. Hydrodynamic and Hydromagnetic Stability. New York: Dover. ISBN 0-486-64071-X.<br /> Chandrasekhar, S. (1987) [1969]. Ellipsoidal Figures of Equilibrium. New York: Dover. ISBN 0-486-65258-0.<br /> Chandrasekhar, S. (1998) [1983]. The Mathematical Theory of Black Holes. New York: Oxford University Press. ISBN 0-19-850370-9.<br /> Chandrasekhar, S. (1990) [1987]. Truth and Beauty. Aesthetics and Motivations in Science. Chicago: The University of Chicago Press. ISBN 0-226-10087-1.<br /> Chandrasekhar, S. (1995). Newton's Principia for the Common Reader. Oxford: Clarendon Press. ISBN 0-19-851744-0.<br /> <br /> <br /> == Nobel Prize ==<br /> <br /> The Nobel Prize in Physics 1983 was divided equally between Subramanyan Chandrasekhar &quot;for his theoretical studies of the physical processes of importance to the structure and evolution of the stars&quot; and William Alfred Fowler &quot;for his theoretical and experimental studies of the nuclear reactions of importance in the formation of the chemical elements in the universe&quot;.<br /> <br /> <br /> == Chandrasekhar limit ==<br /> <br /> This was considered to be his greatest contribution to the world of physics. It is based on theories of black holes and dwarf stars. It is important to the field of astrophysics.<br /> <br /> Using Albert Einstein’s special theory of relativity and the principles of quantum physics, Chandrasekhar showed that it is impossible for a white dwarf star, which is supported solely by a degenerate gas of electrons, to be stable if its mass is greater than 1.44 times the mass of the Sun. If such a star does not completely exhaust its thermonuclear fuel, then this limiting mass may be slightly larger.<br /> <br /> All direct mass determinations of actual white dwarf stars have resulted in masses less than the Chandrasekhar limit. A star that ends its nuclear-burning lifetime with a mass greater than the Chandrasekhar limit must become either a neutron star or a black hole.</div>

Edcunha3 http://www.physicsbook.gatech.edu/index.php?title=Subrahmanyan_Chandrasekhar&diff=12683 2015-12-04T21:55:36Z

<p>Edcunha3: </p> <hr /> <div><br /> == Dragons ==<br /> are cols hs lhvb shvdbr</div>

Edcunha3 http://www.physicsbook.gatech.edu/index.php?title=Subrahmanyan_Chandrasekhar&diff=12682 2015-12-04T21:55:21Z

<p>Edcunha3: Replaced content with &quot; == Dragons ==&quot;</p> <hr /> <div><br /> == Dragons ==</div>

Edcunha3 http://www.physicsbook.gatech.edu/index.php?title=Subrahmanyan_Chandrasekhar&diff=12681 2015-12-04T21:54:33Z

<p>Edcunha3: Created page with &quot;Short Description of Topic Contents [hide] 1 The Main Idea 1.1 A Mathematical Model 1.2 A Computational Model 2 Examples 2.1 Simple 2.2 Middling 2.3 Difficult 3 Connectednes...&quot;</p> <hr /> <div>Short Description of Topic<br /> <br /> Contents [hide] <br /> 1 The Main Idea<br /> 1.1 A Mathematical Model<br /> 1.2 A Computational Model<br /> 2 Examples<br /> 2.1 Simple<br /> 2.2 Middling<br /> 2.3 Difficult<br /> 3 Connectedness<br /> 4 History<br /> 5 See also<br /> 5.1 Further reading<br /> 5.2 External links<br /> 6 References<br /> The Main Idea[edit]<br /> State, in your own words, the main idea for this topic<br /> <br /> <br /> A Mathematical Model[edit]<br /> What are the mathematical equations that allow us to model this topic. For example dp⃗ dtsystem=F⃗ net where p is the momentum of the system and F is the net force from the surroundings.<br /> <br /> A Computational Model[edit]<br /> How do we visualize or predict using this topic. Consider embedding some vpython code here Teach hands-on with GlowScript<br /> <br /> Examples[edit]<br /> Be sure to show all steps in your solution and include diagrams whenever possible<br /> <br /> Simple[edit]<br /> Middling[edit]<br /> Difficult[edit]<br /> Connectedness[edit]<br /> How is this topic connected to something that you are interested in?<br /> How is it connected to your major?<br /> Is there an interesting industrial application?<br /> History[edit]<br /> Put this idea in historical context. Give the reader the Who, What, When, Where, and Why.<br /> <br /> See also[edit]<br /> Are there related topics or categories in this wiki resource for the curious reader to explore? How does this topic fit into that context?<br /> <br /> Further reading[edit]<br /> Books, Articles or other print media on this topic<br /> <br /> External links[edit]<br /> [1]<br /> <br /> <br /> References[edit]<br /> This section contains the the references you used while writing this page</div>

Edcunha3 http://www.physicsbook.gatech.edu/index.php?title=Main_Page&diff=12676 2015-12-04T21:52:23Z

<p>Edcunha3: /* Notable Scientists */</p> <hr /> <div>__NOTOC__<br /> Welcome to the Georgia Tech Wiki for Intro Physics. This resources was created so that students can contribute and curate content to help those with limited or no access to a textbook. When reading this website, please correct any errors you may come across. If you read something that isn't clear, please consider revising it!<br /> <br /> Looking to make a contribution?<br /> #Pick a specific topic from intro physics<br /> #Add that topic, as a link to a new page, under the appropriate category listed below by editing this page.<br /> #Copy and paste the default [[Template]] into your new page and start editing.<br /> <br /> Please remember that this is not a textbook and you are not limited to expressing your ideas with only text and equations. Whenever possible embed: pictures, videos, diagrams, simulations, computational models (e.g. Glowscript), and whatever content you think makes learning physics easier for other students.<br /> <br /> == Source Material ==<br /> All of the content added to this resource must be in the public domain or similar free resource. If you are unsure about a source, contact the original author for permission. That said, there is a surprisingly large amount of introductory physics content scattered across the web. Here is an incomplete list of intro physics resources (please update as needed).<br /> * A physics resource written by experts for an expert audience [https://en.wikipedia.org/wiki/Portal:Physics Physics Portal]<br /> * A wiki book on modern physics [https://en.wikibooks.org/wiki/Modern_Physics Modern Physics Wiki]<br /> * The MIT open courseware for intro physics [http://ocw.mit.edu/resources/res-8-002-a-wikitextbook-for-introductory-mechanics-fall-2009/index.htm MITOCW Wiki]<br /> * An online concept map of intro physics [http://hyperphysics.phy-astr.gsu.edu/hbase/hph.html HyperPhysics]<br /> * Interactive physics simulations [https://phet.colorado.edu/en/simulations/category/physics PhET]<br /> * OpenStax algebra based intro physics textbook [https://openstaxcollege.org/textbooks/college-physics College Physics]<br /> * The Open Source Physics project is a collection of online physics resources [http://www.opensourcephysics.org/ OSP]<br /> * A resource guide compiled by the [http://www.aapt.org/ AAPT] for educators [http://www.compadre.org/ ComPADRE]<br /> <br /> == Organizing Categories ==<br /> These are the broad, overarching categories, that we cover in two semester of introductory physics. You can add subcategories or make a new category as needed. A single topic should direct readers to a page in one of these catagories.<br /> <br /> &lt;div class=&quot;toccolours mw-collapsible mw-collapsed&quot;&gt;<br /> ===Interactions===<br /> &lt;div class=&quot;mw-collapsible-content&quot;&gt;<br /> *[[Kinds of Matter]]<br /> **[[Ball and Spring Model of Matter]]<br /> *[[Detecting Interactions]]<br /> *[[Fundamental Interactions]]<br /> *[[Determinism]]<br /> *[[System &amp; Surroundings]] <br /> *[[Free Body Diagram]]<br /> *[[Newton's First Law of Motion]]<br /> *[[Newton's Second Law of Motion]]<br /> *[[Newton's Third Law of Motion]]<br /> *[[Gravitational Force]]<br /> *[[Electric Force]]<br /> *[[Conservation of Energy]]<br /> *[[Conservation of Charge]]<br /> *[[Terminal Speed]]<br /> *[[Simple Harmonic Motion]]<br /> *[[Speed and Velocity]]<br /> *[[Electric Polarization]]<br /> *[[Perpetual Freefall (Orbit)]]<br /> *[[2-Dimensional Motion]]<br /> *[[Center of Mass]]<br /> *[[Reaction Time]]<br /> *[[Time Dilation]]<br /> &lt;/div&gt;<br /> &lt;/div&gt;<br /> <br /> &lt;div class=&quot;toccolours mw-collapsible mw-collapsed&quot;&gt;<br /> <br /> ===Modeling with VPython===<br /> &lt;div class=&quot;mw-collapsible-content&quot;&gt;<br /> *[[VPython]]<br /> *[[VPython basics]]<br /> *[[VPython Common Errors and Troubleshooting]]<br /> *[[VPython Functions]]<br /> *[[VPython Lists]]<br /> *[[VPython Multithreading]]<br /> &lt;/div&gt;<br /> &lt;/div&gt;<br /> <br /> &lt;div class=&quot;toccolours mw-collapsible mw-collapsed&quot;&gt;<br /> <br /> ===Theory===<br /> &lt;div class=&quot;mw-collapsible-content&quot;&gt;<br /> *[[Einstein's Theory of Special Relativity]]<br /> *[[Einstein's Theory of General Relativity]]<br /> *[[Quantum Theory]]<br /> *[[Maxwell's Electromagnetic Theory]]<br /> *[[Atomic Theory]]<br /> *[[String Theory]]<br /> *[[Elementary Particles and Particle Physics Theory]]<br /> *[[Law of Gravitation]]<br /> &lt;/div&gt;<br /> &lt;/div&gt;<br /> <br /> &lt;div class=&quot;toccolours mw-collapsible mw-collapsed&quot;&gt;<br /> <br /> ===Notable Scientists===<br /> &lt;div class=&quot;mw-collapsible-content&quot;&gt;<br /> *[[Alexei Alexeyevich Abrikosov]]<br /> *[[Christian Doppler]]<br /> *[[Albert Einstein]]<br /> *[[Ernest Rutherford]]<br /> *[[Joseph Henry]]<br /> *[[Michael Faraday]]<br /> *[[J.J. Thomson]]<br /> *[[James Maxwell]]<br /> *[[Robert Hooke]]<br /> *[[Carl Friedrich Gauss]]<br /> *[[Nikola Tesla]]<br /> *[[Andre Marie Ampere]]<br /> *[[Sir Isaac Newton]]<br /> *[[J. Robert Oppenheimer]]<br /> *[[Oliver Heaviside]]<br /> *[[Rosalind Franklin]]<br /> *[[Erwin Schrödinger]]<br /> *[[Enrico Fermi]]<br /> *[[Robert J. Van de Graaff]]<br /> *[[Charles de Coulomb]]<br /> *[[Hans Christian Ørsted]]<br /> *[[Philo Farnsworth]]<br /> *[[Niels Bohr]]<br /> *[[Georg Ohm]]<br /> *[[Galileo Galilei]]<br /> *[[Gustav Kirchhoff]]<br /> *[[Max Planck]]<br /> *[[Heinrich Hertz]]<br /> *[[Edwin Hall]]<br /> *[[James Watt]]<br /> *[[Count Alessandro Volta]]<br /> *[[Josiah Willard Gibbs]]<br /> *[[Richard Phillips Feynman]]<br /> *[[Sir David Brewster]]<br /> *[[Daniel Bernoulli]]<br /> *[[William Thomson]]<br /> *[[Leonhard Euler]]<br /> *[[Robert Fox Bacher]]<br /> *[[Stephen Hawking]]<br /> *[[Amedeo Avogadro]]<br /> *[[Wilhelm Conrad Roentgen]]<br /> *[[Pierre Laplace]]<br /> *[[Thomas Edison]]<br /> *[[Hendrik Lorentz]]<br /> *[[Jean-Baptiste Biot]]<br /> *[[Lise Meitner]]<br /> *[[Lisa Randall]]<br /> *[[Felix Savart]]<br /> *[[Heinrich Lenz]]<br /> *[[Max Born]]<br /> *[[Archimedes]]<br /> *[[Jean Baptiste Biot]]<br /> *[[Carl Sagan]]<br /> *[[Eugene Wigner]]<br /> *[[Marie Curie]]<br /> *[[Pierre Curie]]<br /> *[[Werner Heisenberg]]<br /> *[[Johannes Diderik van der Waals]]<br /> *[[Louis de Broglie]]<br /> *[[Aristotle]]<br /> *[[Émilie du Châtelet]]<br /> *[[Blaise Pascal]]<br /> *[[Benjamin Franklin]]<br /> *[[James Chadwick]]<br /> *[[Henry Cavendish]]<br /> *[[Thomas Young]]<br /> *[[James Prescott Joule]]<br /> *[[John Bardeen]]<br /> *[[Leo Baekeland]]<br /> *[[Alhazen]]<br /> *[[Willebrod Snell]]<br /> *[[Fritz Walther Meissner]]<br /> *[[Johannes Kepler]]<br /> *[[Johann Wilhelm Ritter]]<br /> *[[Philipp Lenard]]<br /> *[[Robert A. Millikan]]<br /> *[[Joseph Louis Gay-Lussac]]<br /> *[[Guglielmo Marconi]]<br /> *[[Luis Walter Alvarez]]<br /> *[[Robert Goddard]]<br /> *[[Léon Foucault]]<br /> *[[Henri Poincaré]]<br /> *[[Steven Weinberg]]<br /> *[[Arthur Compton]]<br /> *[[Pythagoras of Samos]]<br /> *[[Subrahmanyan Chandrasekhar]]<br /> &lt;/div&gt;<br /> &lt;/div&gt;<br /> <br /> &lt;div class=&quot;toccolours mw-collapsible mw-collapsed&quot;&gt;<br /> <br /> ===Properties of Matter===<br /> &lt;div class=&quot;mw-collapsible-content&quot;&gt;<br /> *[[Mass]]<br /> *[[Velocity]]<br /> *[[Relative Velocity]]<br /> *[[Density]]<br /> *[[Charge]]<br /> *[[Spin]]<br /> *[[SI Units]]<br /> *[[Heat Capacity]]<br /> *[[Specific Heat]]<br /> *[[Wavelength]]<br /> *[[Conductivity]]<br /> *[[Malleability]]<br /> *[[Weight]]<br /> *[[Boiling Point]]<br /> *[[Melting Point]]<br /> *[[Inertia]]<br /> *[[Non-Newtonian Fluids]]<br /> *[[Color]]<br /> &lt;/div&gt;<br /> &lt;/div&gt;<br /> <br /> &lt;div class=&quot;toccolours mw-collapsible mw-collapsed&quot;&gt;<br /> <br /> ===Contact Interactions===<br /> &lt;div class=&quot;mw-collapsible-content&quot;&gt;<br /> * [[Young's Modulus]]<br /> * [[Friction]]<br /> * [[Tension]]<br /> * [[Hooke's Law]]<br /> *[[Centripetal Force and Curving Motion]]<br /> *[[Compression or Normal Force]]<br /> * [[Length and Stiffness of an Interatomic Bond]]<br /> * [[Speed of Sound in a Solid]]<br /> * [[Iterative Prediction of Spring-Mass System]]<br /> &lt;/div&gt;<br /> &lt;/div&gt;<br /> <br /> &lt;div class=&quot;toccolours mw-collapsible mw-collapsed&quot;&gt;<br /> <br /> ===Momentum===<br /> &lt;div class=&quot;mw-collapsible-content&quot;&gt;<br /> * [[Vectors]]<br /> * [[Kinematics]]<br /> * [[Conservation of Momentum]]<br /> * [[Predicting Change in multiple dimensions]]<br /> * [[Derivation of the Momentum Principle]]<br /> * [[Momentum Principle]]<br /> * [[Impulse Momentum]]<br /> * [[Curving Motion]]<br /> * [[Projectile Motion]]<br /> * [[Multi-particle Analysis of Momentum]]<br /> * [[Iterative Prediction]]<br /> * [[Analytical Prediction]]<br /> * [[Newton's Laws and Linear Momentum]]<br /> * [[Net Force]]<br /> * [[Center of Mass]]<br /> * [[Momentum at High Speeds]]<br /> * [[Change in Momentum in Time for Curving Motion]]<br /> * [[Momentum with respect to external Forces]]<br /> &lt;/div&gt;<br /> &lt;/div&gt;<br /> <br /> &lt;div class=&quot;toccolours mw-collapsible mw-collapsed&quot;&gt;<br /> <br /> ===Angular Momentum===<br /> &lt;div class=&quot;mw-collapsible-content&quot;&gt;<br /> * [[The Moments of Inertia]]<br /> * [[Moment of Inertia for a ring]]<br /> * [[Rotation]]<br /> * [[Torque]]<br /> * [[Systems with Zero Torque]]<br /> * [[Systems with Nonzero Torque]]<br /> * [[Right Hand Rule]]<br /> * [[Angular Velocity]]<br /> * [[Predicting the Position of a Rotating System]]<br /> * [[Translational Angular Momentum]]<br /> * [[The Angular Momentum Principle]]<br /> * [[Angular Momentum of Multiparticle Systems]]<br /> * [[Rotational Angular Momentum]]<br /> * [[Total Angular Momentum]]<br /> * [[Gyroscopes]]<br /> * [[Angular Momentum Compared to Linear Momentum]]<br /> <br /> &lt;/div&gt;<br /> &lt;/div&gt;<br /> <br /> &lt;div class=&quot;toccolours mw-collapsible mw-collapsed&quot;&gt;<br /> <br /> ===Energy===<br /> &lt;div class=&quot;mw-collapsible-content&quot;&gt;<br /> *[[The Photoelectric Effect]]<br /> *[[Photons]]<br /> *[[The Energy Principle]]<br /> *[[Predicting Change]]<br /> *[[Rest Mass Energy]]<br /> *[[Kinetic Energy]]<br /> *[[Potential Energy]]<br /> **[[Potential Energy for a Magnetic Dipole]]<br /> **[[Potential Energy of a Multiparticle System]]<br /> *[[Work]]<br /> **[[Work Done By A Nonconstant Force]]<br /> *[[Work and Energy for an Extended System]]<br /> *[[Thermal Energy]]<br /> *[[Conservation of Energy]]<br /> *[[Electric Potential]]<br /> *[[Energy Transfer due to a Temperature Difference]]<br /> *[[Gravitational Potential Energy]]<br /> *[[Point Particle Systems]]<br /> *[[Real Systems]]<br /> *[[Spring Potential Energy]]<br /> **[[Ball and Spring Model]]<br /> *[[Internal Energy]]<br /> **[[Potential Energy of a Pair of Neutral Atoms]]<br /> *[[Translational, Rotational and Vibrational Energy]]<br /> *[[Franck-Hertz Experiment]]<br /> *[[Power (Mechanical)]]<br /> *[[Transformation of Energy]]<br /> <br /> *[[Energy Graphs]]<br /> **[[Energy graphs and the Bohr model]]<br /> *[[Air Resistance]]<br /> *[[Electronic Energy Levels]]<br /> *[[Second Law of Thermodynamics and Entropy]]<br /> *[[Specific Heat Capacity]]<br /> *[[The Maxwell-Boltzmann Distribution]]<br /> *[[Electronic Energy Levels and Photons]]<br /> *[[Energy Density]]<br /> *[[Bohr Model]]<br /> *[[Quantized energy levels]]<br /> **[[Spontaneous Photon Emission]]<br /> *[[Path Independence of Electric Potential]]<br /> &lt;/div&gt;<br /> &lt;/div&gt;<br /> <br /> &lt;div class=&quot;toccolours mw-collapsible mw-collapsed&quot;&gt;<br /> <br /> ===Collisions===<br /> &lt;div class=&quot;mw-collapsible-content&quot;&gt;<br /> *[[Collisions]] <br /> Collisions are events that happen very frequently in our day-to-day world. A collision is any sort of process in which before and after a short time interval there is little interaction, but during that short time interval there are large interactions. When looking at collisions, it is first important to understand two very important principles: the Momentum Principle and the Energy Principle. Both principles serve use when talking of collisions because they provide a way in which to analyze these collisions. Collisions themselves can be categorized into 3 main different types: maximally inelastic collisions, elastic collisions, and inelastic collisions. All 3 collisions will get touched on in more detail further on. <br /> *[[Maximally Inelastic Collisions]]<br /> *[[Elastic Collisions]]<br /> *[[Inelastic Collisions]]<br /> *[[Head-on Collision of Equal Masses]]<br /> *[[Head-on Collision of Unequal Masses]]<br /> *[[Frame of Reference]]<br /> *[[Rutherford Experiment and Atomic Collisions]]<br /> *[[Coefficient of Restitution]]<br /> *[[testing123]]<br /> &lt;/div&gt;<br /> &lt;/div&gt;<br /> <br /> &lt;div class=&quot;toccolours mw-collapsible mw-collapsed&quot;&gt;<br /> <br /> ===Fields===<br /> &lt;div class=&quot;mw-collapsible-content&quot;&gt;<br /> * [[Electric Field]] of a<br /> ** [[Point Charge]]<br /> ** [[Electric Dipole]]<br /> ** [[Capacitor]]<br /> ** [[Charged Rod]]<br /> ** [[Charged Ring]]<br /> ** [[Charged Disk]]<br /> ** [[Charged Spherical Shell]]<br /> ** [[Charged Cylinder]]<br /> ** [[Charge Density]]<br /> **[[A Solid Sphere Charged Throughout Its Volume]]<br /> *[[Electric Potential]] <br /> **[[Potential Difference Path Independence]]<br /> **[[Potential Difference in a Uniform Field]]<br /> **[[Potential Difference of point charge in a non-Uniform Field]]<br /> **[[Sign of Potential Difference]]<br /> **[[Potential Difference in an Insulator]]<br /> **[[Energy Density and Electric Field]]<br /> ** [[Systems of Charged Objects]]<br /> *[[Electric Force]]<br /> *[[Polarization]]<br /> **[[Polarization of an Atom]]<br /> *[[Charge Motion in Metals]]<br /> *[[Charge Transfer]]<br /> *[[Magnetic Field]]<br /> **[[Right-Hand Rule]]<br /> **[[Direction of Magnetic Field]]<br /> **[[Magnetic Field of a Long Straight Wire]]<br /> **[[Magnetic Field of a Loop]]<br /> **[[Magnetic Field of a Solenoid]]<br /> **[[Bar Magnet]]<br /> **[[Magnetic Dipole Moment]]<br /> ***[[Stern-Gerlach Experiment]]<br /> **[[Magnetic Force]]<br /> **[[Earth's Magnetic Field]]<br /> **[[Atomic Structure of Magnets]]<br /> *[[Combining Electric and Magnetic Forces]]<br /> **[[Magnetic Torque]]<br /> **[[Hall Effect]]<br /> **[[Lorentz Force]]<br /> **[[Biot-Savart Law]]<br /> **[[Biot-Savart Law for Currents]]<br /> **[[Integration Techniques for Magnetic Field]]<br /> **[[Sparks in Air]]<br /> **[[Motional Emf]]<br /> **[[Detecting a Magnetic Field]]<br /> **[[Moving Point Charge]]<br /> **[[Non-Coulomb Electric Field]]<br /> **[[Motors and Generators]]<br /> **[[Solenoid Applications]]<br /> &lt;/div&gt;<br /> &lt;/div&gt;<br /> <br /> &lt;div class=&quot;toccolours mw-collapsible mw-collapsed&quot;&gt;<br /> <br /> ===Simple Circuits===<br /> &lt;div class=&quot;mw-collapsible-content&quot;&gt;<br /> *[[Components]]<br /> *[[Steady State]]<br /> *[[Non Steady State]]<br /> *[[Charging and Discharging a Capacitor]]<br /> *[[Thin and Thick Wires]]<br /> *[[Node Rule]]<br /> *[[Loop Rule]]<br /> *[[Resistivity]]<br /> *[[Power in a circuit]]<br /> *[[Ammeters,Voltmeters,Ohmmeters]]<br /> *[[Current]]<br /> **[[AC]]<br /> *[[Ohm's Law]]<br /> *[[Series Circuits]]<br /> *[[Parallel Circuits]]<br /> *[[RC]]<br /> *[[AC vs DC]]<br /> *[[Charge in a RC Circuit]]<br /> *[[Current in a RC circuit]]<br /> *[[Circular Loop of Wire]]<br /> *[[Current in a RL Circuit]]<br /> *[[RL Circuit]]<br /> *[[LC Circuit]]<br /> *[[Surface Charge Distributions]]<br /> *[[Feedback]]<br /> *[[Transformers (Circuits)]]<br /> *[[Resistors and Conductivity]]<br /> *[[Semiconductor Devices]]<br /> &lt;/div&gt;<br /> &lt;/div&gt;<br /> <br /> &lt;div class=&quot;toccolours mw-collapsible mw-collapsed&quot;&gt;<br /> <br /> ===Maxwell's Equations===<br /> &lt;div class=&quot;mw-collapsible-content&quot;&gt;<br /> *[[Gauss's Flux Theorem]]<br /> **[[Electric Fields]]<br /> ***[[Examples of Flux Through Surfaces and Objects]]<br /> **[[Magnetic Fields]]<br /> *[[Ampere's Law]]<br /> **[[Magnetic Field of Coaxial Cable Using Ampere's Law]]<br /> **[[Magnetic Field of a Long Thick Wire Using Ampere's Law]]<br /> **[[Magnetic Field of a Toroid Using Ampere's Law]]<br /> *[[Faraday's Law]]<br /> **[[Curly Electric Fields]]<br /> **[[Inductance]]<br /> ***[[Transformers (Physics)]]<br /> ***[[Energy Density]]<br /> **[[Lenz's Law]]<br /> ***[[Lenz Effect and the Jumping Ring]]<br /> **[[Lenz's Rule]]<br /> **[[Motional Emf using Faraday's Law]]<br /> *[[Ampere-Maxwell Law]]<br /> *[[Superconductors]]<br /> **[[Meissner effect]]<br /> &lt;/div&gt;<br /> &lt;/div&gt;<br /> <br /> &lt;div class=&quot;toccolours mw-collapsible mw-collapsed&quot;&gt;<br /> <br /> ===Radiation===<br /> &lt;div class=&quot;mw-collapsible-content&quot;&gt;<br /> *[[Producing a Radiative Electric Field]]<br /> *[[Sinusoidal Electromagnetic Radiaton]]<br /> *[[Lenses]]<br /> *[[Energy and Momentum Analysis in Radiation]]<br /> **[[Poynting Vector]]<br /> *[[Electromagnetic Propagation]]<br /> **[[Wavelength and Frequency]]<br /> *[[Snell's Law]]<br /> *[[Effects of Radiation on Matter]]<br /> *[[Light Propagation Through a Medium]]<br /> *[[Light Scaterring: Why is the Sky Blue]]<br /> *[[Light Refraction: Bending of light]]<br /> *[[Cherenkov Radiation]]<br /> &lt;/div&gt;<br /> &lt;/div&gt;<br /> &lt;div class=&quot;toccolours mw-collapsible mw-collapsed&quot;&gt;<br /> <br /> ===Sound===<br /> &lt;div class=&quot;mw-collapsible-content&quot;&gt;<br /> *[[Doppler Effect]]<br /> *[[Nature, Behavior, and Properties of Sound]]<br /> *[[Resonance]]<br /> *[[Sound Barrier]]<br /> &lt;/div&gt;<br /> &lt;/div&gt;<br /> &lt;div class=&quot;toccolours mw-collapsible mw-collapsed&quot;&gt;<br /> <br /> ===Waves===<br /> &lt;div class=&quot;mw-collapsible-content&quot;&gt;<br /> *[[Multisource Interference: Diffraction]]<br /> *[[Standing waves]]<br /> *[[Gravitational waves]]<br /> *[[Plasma waves]]<br /> *[[Wave-Particle Duality]]<br /> *[[Electromagnetic Waves]]<br /> *[[Electromagnetic Spectrum]]<br /> *[[Color Light Wave]]<br /> *[[Mechanical Waves]]<br /> *[[Pendulum Motion]]<br /> *[[Transverse and Longitudinal Waves]]<br /> *[[Planck's Relation]]<br /> &lt;/div&gt;<br /> &lt;/div&gt;<br /> &lt;div class=&quot;toccolours mw-collapsible mw-collapsed&quot;&gt;<br /> <br /> ===Real Life Applications of Electromagnetic Principles===<br /> &lt;div class=&quot;mw-collapsible-content&quot;&gt;<br /> *[[Electromagnetic Junkyard Cranes]]<br /> *[[Maglev Trains]]<br /> *[[Spark Plugs]]<br /> *[[Metal Detectors]]<br /> *[[Speakers]]<br /> *[[Radios]]<br /> *[[Ampullae of Lorenzini]]<br /> *[[Electrocytes]]<br /> *[[Generator]]<br /> &lt;/div&gt;<br /> &lt;/div&gt;<br /> <br /> &lt;div class=&quot;toccolours mw-collapsible mw-collapsed&quot;&gt;<br /> <br /> ===Optics===<br /> &lt;div class=&quot;mw-collapsible-content&quot;&gt;<br /> *[[Mirrors]]<br /> *[[Refraction]]<br /> *[[Quantum Properties of Light]]<br /> &lt;/div&gt;<br /> &lt;/div&gt;<br /> <br /> == Resources ==<br /> * Commonly used wiki commands [https://en.wikipedia.org/wiki/Help:Cheatsheet Wiki Cheatsheet]<br /> * A guide to representing equations in math mode [https://en.wikipedia.org/wiki/Help:Displaying_a_formula Wiki Math Mode]<br /> * A page to keep track of all the physics [[Constants]]<br /> * A page for review of [[Vectors]] and vector operations</div>

Edcunha3