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His books covered such diverse topics as astronomy, cryptology and atomic physics. In 2005, Kippenhahn was honoured by the Royal Astronomical Society with the Eddington medal for his scientific research into the computation of the structure of star and of stellar evolution.
Stellar evolution is the process by which a star changes over the course of its lifetime and how it can lead to the creation of a new star. Depending on the mass of the star, its lifetime can range from a few million years for the most massive to trillions of years for the least massive, which is considerably longer than the current age of the ...
Schwarzschild's work in the fields of stellar structure and stellar evolution led to improved understanding of pulsating stars, differential solar rotation, post-main sequence evolutionary tracks on the Hertzsprung-Russell diagram (including how stars become red giants), hydrogen shell sources, the helium flash, and the ages of star clusters.
Subrahmanyan Chandrasekhar (/ 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.
This results in compositional evolution of cosmic gas in and between stars and galaxies, enriching such gas with heavier elements. Nuclear astrophysics is the science to describe and understand the nuclear and astrophysical processes within such cosmic and galactic chemical evolution, linking it to knowledge from nuclear physics and astrophysics.
In stellar astronomy, the Algol paradox is a paradoxical situation when elements of a binary star seem to evolve in discord with the established theories of stellar evolution. [1] A fundamental feature of these theories is that the rate of evolution of stars depends on their mass: The greater the mass, the faster this evolution, and the more ...
Roberta M. Humphreys is an American observational stellar astrophysicist. She is Professor Emerita at the University of Minnesota.Her work has included Galactic structure, observational stellar evolution, stellar populations, and large databases.
Stellar evolution tracks (blue lines) for the pre-main-sequence. The nearly vertical curves are Hayashi tracks. Low-mass stars have nearly vertical evolution tracks until they arrive on the main sequence. For more-massive stars, the Hayashi track bends to the left into the Henyey track. Even more-massive stars are born directly onto the Henyey ...