Chandrasekhar limit

The Chandrasekhar limit is the maximum mass of a stable white dwarf star. The limit was first published by Wilhelm Anderson and E. C. Stoner, and was named after Subrahmanyan Chandrasekhar, the Indian-American astrophysicist who improved upon the accuracy of the calculation in 1930, at the age of 19. 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, unlike main sequence stars, resist gravitational collapse primarily through electron degeneracy pressure, rather than 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.
== Tossup Questions ==
# One analog of this concept is named after Tolman, Oppenheimer, and Volkov. Its namesake solved three cases of the Lane-Emden equation. The denominator of the formula used to calculate it includes the square of the number of nucleons per electron, and Schonberg's name is sometimes appended to it. Equal to approximately 1.4 solar masses, for 10 points, name this theoretical maximum mass a white dwarf can obtain before collapsing in on itself and forming a black hole, a limit named after an Indian physicist.
# In 1987, Lieb and Yau proposed an analog of this for boson-composed stars such as axion stars, using a Hartree-type equation instead of the namesake's. As a consequence of it, main sequence stars larger than eight solar masses must become neutron stars or black holes. The value for it is thought to be around 1.4 solar masses or 2.96x1030 [2.96 times 10 to the 30th] kilograms, and no white dwarf can be stabilized by degeneracy pressure beyond it. For 10 points, identify this mass limit named for an Indian astrophysicist.