The Chandrasekhar limit ( ) is the maximum mass of a stable white dwarf star.
 The limit was first indicated in papers published by Wilhelm Anderson and E. C. Stoner, and was named after Subrahmanyan Chandrasekhar, the Indian astrophysicist who independently discovered and improved upon the accuracy of the calculation in 1930, at the age of 19, in India.
 This 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.
 White dwarfs resist gravitational collapse primarily through electron degeneracy pressure.
 (By comparison, main sequence stars 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, white dwarfs with masses greater than the limit would be subject to further gravitational collapse, evolving into a different type of stellar remnant, such as a neutron star or black hole.
 (However, white dwarfs generally avoid this fate by exploding before they undergo collapse.)
 Those with masses under the limit remain stable as white dwarfs.
In astrophysics, Chandrasekhar potential energy tensor provides the gravitational potential of a body due to its own gravity created by the distribution of matter across the body, named after the Indian American astrophysicist Subrahmanyan Chandrasekhar.
 The Chandrasekhar tensor is a generalization of potential energy in other words, the trace of the Chandrasekhar tensor provides the potential energy of the body.
In stellar astrophysics, the Schönberg–Chandrasekhar limit is the maximum mass of a non-fusing, isothermal core that can support an enclosing envelope.
 It is expressed as the ratio of the core mass to the total mass of the core and envelope.
 Estimates of the limit depend on the models used and the assumed chemical compositions of the core and envelope; typical values given are from 0.10 to 0.15 (10% to 15% of the total stellar mass).
 This is the maximum to which a helium-filled core can grow, and if this limit is exceeded, as can only happen in massive stars, the core collapses, releasing energy that causes the outer layers of the star to expand to become a red giant.
 It is named after the astrophysicists Subrahmanyan Chandrasekhar and Mario Schönberg, who estimated its value in a 1942 paper.
The Chandrasekhar family is an Indian intellectual family.
 Several members of the family have achieved scientific distinction, notably in the field of physics.
 Two members of the family, Sir C. V. Raman and his nephew, Subrahmanyan Chandrasekhar, were Nobel laureates in physics.
Subrahmanyan Chandrasekhar, FRS (Tamil: சுப்பிரமணியன் சந்திரசேகர் ; ; 19 October 1910 – 21 August 1995), was an Indian American astrophysicist who was awarded the 1983 Nobel Prize for Physics with William A. Fowler "for his theoretical studies of the physical processes of importance to the structure and evolution of the stars".
 His mathematical treatment of stellar evolution yielded many of the best current theoretical models of the later evolutionary stages of massive stars and black holes.
 The Chandrasekhar limit is named after him.
Collapsar is the shortened form to describe a collapsed star.
 When an old star no longer has enough fuel for significant fusion reactions there can be three possible outcomes depending on the star's mass.
 If the star’s mass is less than 1.4 solar masses, known as the Chandrasekhar limit, it will stabilize and shrink, becoming a white dwarf.
 Above the said limit the star will either become a neutron star or a black hole.
In astrophysics, the Chandrasekhar equation is a dimensionless form of the Poisson equation for the density distribution of a spherically symmetric isothermal gas sphere subjected to its own gravitaional force, named after the Indian American astrophysicist Subrahmanyan Chandrasekhar.
 The equation reads
This is a list of supernova candidates, or stars that astronomers have suggested are supernova progenitors.
 Type II supernova progenitors include stars with at least 10 solar masses that are in the final stages of their evolution.
 Prominent examples of stars in this mass range include Antares, Spica, Gamma Velorum, Mu Cephei, and members of the Quintuplet Cluster.
 Type Ia supernova progenitors are white dwarf stars that are close to the Chandrasekhar limit of about 1.44 solar masses and are accreting matter from a binary companion star.
 The list includes massive Wolf–Rayet stars, which may become Type Ib/Ic supernovae.
The Tolman–Oppenheimer–Volkoff limit (or TOV limit) (also referred to as the Landau–Oppenheimer–Volkoff limit (or LOV limit)) is an upper bound to the mass of stars composed of neutron-degenerate matter (i.e. neutron stars).
 The TOV limit is analogous to the Chandrasekhar limit for white dwarf stars.
 It is approximately 1.5 to 3.0 solar masses, corresponding to an original stellar mass of 15 to 20 solar masses.
KPD 1930+2752 is a binary star system including a Subdwarf B star and a probable white dwarf with relatively high mass.
 Due to the nature of this astronomical system, it seems like a likely candidate for a potential type Ia supernova, a type of supernova which occurs when a white dwarf star takes on enough matter to approach the Chandrasekhar limit, the point at which electron degeneracy pressure would not be enough to support its mass.
 However, carbon fusion would occur before this limit was reached, releasing enough energy to overcome the force of gravity holding the star together and resulting in a supernova.

Question: The Chandrasekhar limit was named after an astrophysicist, what is the name of his uncle of which is also a novel laureate?
Answer: Sir C. V. Raman