Why Chandrasekhar Limit matters in Astrophysics!

Hey, if you are active in space, then you may know about Black Holes and Dwarfs, then you may heard about Chandrasekhar Limit, well if you don’t then after this reading you will so

Subrahmanyan Chandrasekhar was one of best mind from India, he was a physicist, who figured out what the maximum mass of dwarf and from which mass we can state the object is black hole. (For which he get the Nobel Prize in 1983 and shared with William.A. Fowler.

Chandrasekhar Limit is a barrier which indicates the maximum mass of any stable dwarf star. It means any mass bigger than this will become definite a singularity in near time.

The currently accepted value of limit is 1.4 M☉. Any mass bigger than this is black hole, (it’s very worthy to bet). White Dwarf resist the collapse because of thermal pressure. But when mass becomes bigger thermal pressure reduces, and gravitational collapse is seems likely to happen. But masses less than this barrier is safe, that’s means pluto is safe (1.0004 M).

Theoretically it was reduced from Fermi gas,

{\displaystyle M_{\rm {limit}}={\frac {\omega _{3}^{0}{\sqrt {3\pi }}}{2}}\left({\frac {\hbar c}{G}}\right)^{\frac {3}{2}}{\frac {1}{(\mu _{\text{e}}m_{\text{H}})^{2}}}}

This equation states the limit, but the idea of this blog is simplicity, so we have to stick with best concept without complex equations.

Well if you will talk about the application then look, In April 2003, the Supernova Legacy Survey observed a type Ia supernova, designated SNLS-03D3bb, in a galaxy approximately 4 billion light years away. According to a group of astronomers at the University of Toronto and elsewhere, the observations of this supernova are best explained by assuming that it arose from a white dwarf that grew to twice the mass of the Sun before exploding.

They believe that the star, dubbed the “Champagne Supernova” by University of Oklahoma astronomer David R. Branch, may have been spinning so fast that a centrifugal tendency allowed it to exceed the limit. Alternatively, the supernova may have resulted from the merger of two white dwarfs, so that the limit was only violated momentarily. Nevertheless, they point out that this observation poses a challenge to the use of type Ia supernovae as standard candles. – Credit to Wikipidea Article.

Look at the graph of limit,

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