** Chandrasekhar

** Chandrasekhar limit, an astrophysics formula named for him.

** Chandrasekhar number, an astrophysics quantity also named for him.

** Physics – Subrahmanyan Chandrasekhar, William Alfred Fowler

** Some kinds of helicity are conserved in dissipationless limit: hydrodynamical helicity, magnetic helicity, cross-helicity.

** The set of infinite strings is the inverse limit of the set of finite strings, and is thus endowed with the limit topology.

** One-sided limit

** Limit superior and limit inferior

** Direct limit and Inverse limit

** Greisen – Zatsepin – Kuzmin limit

** Speed limit

** The high-frequency limit of the hearing range

** A limit order is a type of order to buy a security at no more ( or sell at no less ) than a specific price on an exchange.

** Engine piston rings changed to limit oil consumption and pistons changed to strengthen skirt area.

** A Line reactor is used to limit starting current of motors and to protect variable frequency drives

** The United States Senate adopts the cloture rule in order to limit filibusters.

** The first speed limit is introduced in Britain: in town and in the country.

** A speed limit is imposed on British roads.

** See more fully the discussion in Dennis J. Baker, The Right Not to be Criminalized: Demarcating Criminal Law's Authority ( Ashgate, 2011 < http :// www. ashgate. com / isbn / 9781409427650 >) where Professor Baker argues ( in chapter 5 ) that there is a limit to consensual harm doing — but that the threshold of harm has to be reasonably high.

** Lower limit: 70-80 modal ( bass ), 30-40 creaky

** Upper limit: 1170 ( soprano )

** Railroad adze-A carpenter's adze which had its bit extended in an effort to limit the breaking of handles when shaping railroad ties ( railway sleepers ).

** Lyapunov's central limit theorem

** serum creatinine ≥ 2 times the upper limit of normal for age or 2-fold increase in baseline creatinine in patients with chronic kidney disease

** alanine aminotransferase ( ALT ) ≥ 2 times the upper limit of normal

** A lossless " PCM macroblock " representation mode in which video data samples are represented directly, allowing perfect representation of specific regions and allowing a strict limit to be placed on the quantity of coded data for each macroblock.

In 1931, Subrahmanyan Chandrasekhar calculated, using special relativity, that a non-rotating body of electron-degenerate matter above a certain limiting mass ( now called the Chandrasekhar limit at 1. 4 solar masses ) has no stable solutions.

They were partly correct: a white dwarf slightly more massive than the Chandrasekhar limit will collapse into a neutron star, which is itself stable because of the Pauli exclusion principle.

But in 1939, Robert Oppenheimer and others predicted that neutron stars above approximately three solar masses ( the Tolman – Oppenheimer – Volkoff limit ) would collapse into black holes for the reasons presented by Chandrasekhar, and concluded that no law of physics was likely to intervene and stop at least some stars from collapsing to black holes.

The Chandrasekhar limit () is the maximum mass of a stable white dwarf star.

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.

This is the Chandrasekhar limit.

After a talk by Chandrasekhar on the limit in 1935, he replied:

If a main-sequence star is not too massive ( less than approximately 8 solar masses ), it will eventually shed enough mass to form a white dwarf having mass below the Chandrasekhar limit, which will consist of the former core of the star.

It has been inferred that as the white dwarf's mass approaches the Chandrasekhar limit, its central density increases, and, as a result of compressional heating, its temperature also increases.

Since the observation of the Champagne Supernova in 2003, more very bright type Ia supernovae are thought to have originated by white dwarfs whose masses exceeded the Chandrasekhar limit.

The limit of neutron degeneracy pressure, analogous to the Chandrasekhar limit, is known as the Tolman – Oppenheimer – Volkoff limit.

* White dwarf stars and the Chandrasekhar limit, Masters ' thesis, Dave Gentile, DePaul University, 1995.

Eventually, the white dwarf could explode as a type Ia supernova if it approaches the Chandrasekhar limit.

In general, compact stars of less than 1. 38 solar masses – the Chandrasekhar limit – are white dwarfs, and above 2 to 3 solar masses ( the Tolman – Oppenheimer – Volkoff limit ), a quark star might be created ; however, this is uncertain.

If the mass of the core exceeds the Chandrasekhar limit, electron degeneracy pressure will be unable to support its weight against the force of gravity, and the core will undergo sudden, catastrophic collapse to form a neutron star or ( in the case of cores that exceed the Tolman-Oppenheimer-Volkoff limit ), a black hole.

As another example of its many applications, the virial theorem has been used to derive the Chandrasekhar limit for the stability of white dwarf stars.

The physics of degeneracy yields a maximum mass for a non-rotating white dwarf, the Chandrasekhar limit — approximately 1. 4 solar masses — beyond which it cannot be supported by electron degeneracy pressure.

In extreme cases this event can cause the white dwarf to exceed the Chandrasekhar limit and trigger a supernova that destroys the entire star, and is another possible cause for runaways.

The supernova explosion is caused by a white dwarf or a star core reaching a certain mass / density limit, the Chandrasekhar limit, causing the object to collapse in a fraction of a second.