what is chandrasekhar limit in astronomy?

Question

useful in space researches.proposed by an indian astronomer Chandrasekhar:hence it is named. he got Nobel Prize for this

Answer 1

The Chandrasekhar limit (named after Subrahmanyan Chandrasekhar) is the maximum nonrotating mass which can be supported against gravitational collapse by electron degeneracy pressure. It is commonly given as being about 1.4 or 1.44 solar masses. Computed values for the limit will vary depending on the nuclear composition of the mass and the approximations used.
As white dwarf stars are supported by electron degeneracy pressure, this is an upper limit for the mass of a white dwarf. Main-sequence stars with a mass exceeding approximately 8 solar masses therefore cannot lose enough mass to form a stable white dwarf at the end of their lives, and instead form either a neutron star or black hole.

I hope I've been helpful!!

Answer 2

The Chandrasekhar Limit, named after an Indian Nobel Prize winner, is a limiting mass:
a) below which: a star can becaome a white dwarf (these are stars with moderate and low masses, like the sun)
b) and above ehich: gravity is capable of continuing the collapse into a neutron star or black hole (those with high masses)

It actually is a tool in determining the eventual fate of a star.

Answer 3

The Chandrasekhar limit is named after Subrahmanyan Chandrasekhar from India I believe. It is is the maximum nonrotating mass which can be supported against gravitational collapse by electron degeneracy pressure. It is about 1.4 or 1.44 solar masses. Computed values for the limit will vary depending on the nuclear composition of the mass and the approximations used.

Answer 4

The Chandrasekhar limit (named after Subrahmanyan Chandrasekhar) is the maximum nonrotating mass which can be supported against gravitational collapse by electron degeneracy pressure. It is commonly given as being about 1.4 or 1.44 solar masses. Computed values for the limit will vary depending on the nuclear composition of the mass and the approximations used. Chandrasekhar[1], eq. (36),[2], eq. (58),[3], eq. (43) gives a value of

\frac{\omega_3^0 \sqrt{3\pi}}{2}\left ( \frac{\hbar c}{G}\right )^{3/2}\frac{1}{(\mu_e m_H)^2}.

Here, μe is the average molecular weight per electron, mH is the mass of the hydrogen atom, and \omega_3^0 \approx 2.018236 is a constant connected with the solution to the Lane-Emden equation. Numerically, this value is approximately (2/μe)2 · 2.85 · 1030 kg, or 1.43 (2/\mu_e)^2 M_{\bigodot}, where M_{\bigodot}=1.989\cdot 10^{30} \ {\rm kg} is the standard solar mass.[4] As \sqrt{\hbar c/G} is the Planck mass, M_{\rm Pl}\approx 2.176\cdot 10^{-8}\ {\rm kg}, the limit is of the order of MPl3/mH2.

As white dwarf stars are supported by electron degeneracy pressure, this is an upper limit for the mass of a white dwarf. Main-sequence stars with a mass exceeding approximately 8 solar masses therefore cannot lose enough mass to form a stable white dwarf at the end of their lives, and instead form either a neutron star or black hole.[5][6][7]

Answer 5

1.4 solar masses is about the maximum a white dwarf can remain a white dwarf without becoming a neutron star.