The Chandrasekhar limit (/tʃʌndrəˈseɪkər/) is the maximum mass of a stable white dwarf star. The currently accepted value of the Chandrasekhar limit is about 1.4 M☉ (2.765×1030 kg). White dwarfs resist gravitational collapse primarily through electron degeneracy pressure, compared to main sequence stars, which resist collapse through thermal pressure. The Chandrasekhar limit is the mass above which electron degeneracy pressure in the star's core is insufficient to balance the star's own gravitational self-attraction. Consequently, a white dwarf with a mass greater than the limit is subject to further gravitational collapse, evolving into a different type of stellar remnant, such as a neutron star or black hole. Those with masses up to the limit remain stable as white dwarfs. Tolman–Oppenheimer–Volkoff limit is theoretically a next level to reach in order for a neutron star to collapse into a denser form such as a black hole. The limit was named after Subrahmanyan Chandrasekhar. Chandrasekhar improved upon the accuracy of the calculation in 1930 by calculating the limit for a polytrope model of a star in hydrostatic equilibrium, and comparing his limit to the earlier limit found by E. C. Stoner for a uniform density star. Importantly, the existence of a limit, based on the conceptual breakthrough of combining relativity with Fermi degeneracy, was indeed first established in separate papers published by Wilhelm Anderson and E. C. Stoner in 1929. The limit was initially ignored by the community of scientists because such a limit would logically require the existence of black holes, which were considered a scientific impossibility at the time. The fact that the roles of Stoner and Anderson are often overlooked in the astronomy community has been noted. (Wikipedia).
What is the Chandrasekhar limit for White Dwarf Stars?
This video provides a simplified step by step derivation of the Chandrasekhar limit for White Dwarf stars. After briefly discussing the history of white dwarf stars, an overview of electron degeneracy pressure is provided. Using a combination of quantum mechanics and Einstein's theory of s
From playlist Relativity
Teach Astronomy - Chandrasekhar Limit
http://www.teachastronomy.com/ White dwarfs cannot have a larger mass than about 1.4 times the mass of the Sun because above this mass the white dwarf structure becomes unstable; gravity overcomes the degeneracy pressure of the electrons and further collapse occurs. This is called the Cha
From playlist 16. Stars 3
Astronomy: The Supernova (6 of 10) Chandrasekhar Limit
Visit http://ilectureonline.com for more math and science lectures! In this video I will explain what are chandrasekhar limits.
From playlist ASTRONOMY 20 SUPERNOVA - THE DEATH OF STARS
Limit of (4u^4 + 5)/((u^2 - 2)(2u^2 - 1)) as u approaches infinity
Limit of (4u^4 + 5)/((u^2 - 2)(2u^2 - 1)) as u approaches infinity. This is a calculus problem where we find a limit as u approaches infinity. In this case we have a rational function and the numerator and denominator have the same growth rate, so the limit is the ratio of the leading coef
From playlist Limits at Infinity
The limit is the limit is the limit is the limit
Here I evaluate a neat infinite limit with l'Hopital's rule... does it work though? Subscribe to my channel: https://youtube.com/drpeyam Check out my TikTok channel: https://www.tiktok.com/@drpeyam Follow me on Instagram: https://www.instagram.com/peyamstagram/ Follow me on Twitter: https
From playlist Calculus
Ex: Limits at Infinity of a Function Involving an Exponential Function
This video provides two examples of how to determine limits at infinity of a function involving a square root. The results are verified graphically. Site: http://mathispower4u.com Blog: http://mathispower4u.wordpress.com
From playlist Limits at Infinity and Special Limits
Chandrasekhar LIMIT - Universe Sandbox 2
Support this channel on Patreon: https://www.patreon.com/user?u=2318196&ty=h Hello and welcome to What Da Math! In this video, we will talk about Chandra limit and the person who is responsible for discovering it. This video will help you understand white dwarfs a little bit better and w
From playlist Universe Sandbox 2
Ex: Limits at Infinity of a Rational Function (DNE)
This video provides two examples of how to determine limits at infinity of a rational function when the limits to not exist. The results are verified graphically. Site: http://mathispower4u.com Blog: http://mathispower4u.wordpress.com
From playlist Limits at Infinity and Special Limits
http://www.teachastronomy.com/ A supernova is the violently explosive death of a star with the corresponding release of radiant energy, a flood of neutrinos, and the creation and ejection of heavy elements into space, the most spectacular phenomena in astronomy. Supernovae can occur in tw
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Calculus 2.4 The Precise Definition of a Limit
My notes are available at http://asherbroberts.com/ (so you can write along with me). Calculus: Early Transcendentals 8th Edition by James Stewart
From playlist Calculus
http://www.teachastronomy.com/ A supernova is the violently explosive death of a star with the corresponding release of radiant energy, a flood of neutrinos, and the creation and ejection of heavy elements into space, the most spectacular phenomena in astronomy. Supernovae can occur in tw
From playlist 17. Galactic Mass Distribtuion and Galaxy Structure
New Caltech Study Suggests We Were Wrong About White Dwarf Supernovae
You can buy Universe Sandbox 2 game here: http://amzn.to/2yJqwU6 Hello and welcome! My name is Anton and in this video, we will talk about new research that suggests some white dwarf stars don't behave as they should and that the size of the universe might be in question. Paper: https://a
From playlist Supernovae
Limits At Infinity - Additional Examples
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From playlist Limits
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Summer course 2018 - A Random walk in astro-physics Lecture - 10 : Quantum Stars (Lecture - 10) by G Srinivasan 10.00 to 12.00 Friday, 15 June 2018 Madhava Lecture Hall, ICTS Bangalore The range of densities, temperatures, magnetic fields, etc. that obtain in the Universe are staggerin
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S. Chandrasekhar's fluid dynamics by Katepalli Raju Sreenivasan
DATE: 23 January 2018, 16:00 to 17:00 VENUE: Ramanujan Lecture Hall, ICTS Bangalore Lecture 1: 22 January 2018, 16:00 to 17:00 Title: Chandra's fluid dynamics Abstract: This talk will describe and assess S. Chandrasekhar's work in fluid dynamics from about 1948 to 1960 and include remar
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Neutron Stars and Black Holes (Lecture - 02: White Dwarf Stars) by G Srinivasan
SUMMER COURSES NEUTRON STARS AND BLACK HOLES SPEAKER: G Srinivasan (Raman Research Institute - Retired) DATE: 15 May 2019 to 28 June 2019 VENUE: Emmy Noether Seminar Room, ICTS Bangalore The theme of the course will be neutron stars and black holes, with emphasis on neutron stars i
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This video introduces limits at infinity. https://mathispower4u.com
From playlist Limits at Infinity and Special Limits
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Summer School on Gravitational-Wave Astronomy DATE: 17 July 2017 to 28 July 2017 VENUE: Madhava Lecture Hall, ICTS Bangalore This school is a part of the annual ICTS summer schools in gravitational wave astronomy. This year’s school will focus on the physics and astrophysics of compact
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