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In astrophysics, dynamical friction or Chandrasekhar friction, sometimes called gravitational drag, is loss of momentum and kinetic energy of moving bodies through gravitational interactions with surrounding matter in space. It was first discussed in detail by Subrahmanyan Chandrasekhar in 1943. [1] [2] [3]
Subrahmanyan Chandrasekhar FRS (/ ˌ tʃ ə n d r ə ˈ ʃ eɪ k ər /; [3] 19 October 1910 – 21 August 1995) [4] was an Indian-American theoretical physicist who made significant contributions to the scientific knowledge about the structure of stars, stellar evolution and black holes.
And inside such a typical galaxy the dynamical friction and accretion on stellar black holes over a 10-Gyr Hubble time change the black hole's velocity and mass by only an insignificant fraction % if the black hole makes up less than 0.1% of the total galaxy mass N M ⊙ ∼ 10 6 − 11 M ⊙ {\displaystyle NM_{\odot }\sim 10^{6-11}M_{\odot }} .
In atmospheric radiation, Chandrasekhar's X- and Y-function appears as the solutions of problems involving diffusive reflection and transmission, ...
The contents of this article is a list of things named after the Indian-American theoretical physicist Subrahmanyan Chandrasekhar. Chandrasekhar limit [1] Chandrasekhar friction; Chandrasekhar polarization; Chandrasekhar–Kendall function; Chandrasekhar's H-function; Schönberg–Chandrasekhar limit; Velikhov–Chandrasekhar instability
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The Chandrasekhar limit (/ ˌ tʃ ə n d r ə ˈ ʃ eɪ k ər /) [1] is the maximum mass of a stable white dwarf star. The currently accepted value of the Chandrasekhar limit is about 1.4 M ☉ ( 2.765 × 10 30 kg ).
Chandrasekhar's H-function for different albedo. In atmospheric radiation, Chandrasekhar's H-function appears as the solutions of problems involving scattering, introduced by the Indian American astrophysicist Subrahmanyan Chandrasekhar.