Published March 30, 2007
by Springer .
Written in English
|Contributions||A.K. Dupree (Editor), Maria Teresa Vaz Torrão Lago (Editor)|
|The Physical Object|
|Number of Pages||478|
Since we saw that low-mass stars are much more common than high-mass stars, this confirms our view of planetary nebulae as sort of “last gasp” of low-mass star evolution. Cosmic Recycling The loss of mass by dying stars is a key step in the gigantic cosmic recycling scheme we discussed in Between the Stars: Gas and Dust in Space. Calculations showing that white dwarfs are the likely end state of low-mass stars were first carried out by the Indian-American astrophysicist Subrahmanyan Chandrasekhar. He was able to show how much a star will shrink before the degenerate electrons halt its further contraction and hence what its final diameter will be (Figure ). The physics of star formation while the evolution of galaxies depends on the spectrum of masses with which they form, since low-mass stars are faint and evolve slowly while massive ones evolve fast and release large amounts of matter and energy that can heat. item 3 Formation and Evolution of Low Mass Stars (English) Hardcover Book Free Shipping - Formation and Evolution of Low Mass Stars (English) Hardcover Book Free Shipping. $ Free shipping. No ratings or reviews yet. Be the first to write a review. Best Selling in Nonfiction. See all.
Based on these principles, the evolution of low- and high-mass stars is explained from their formation to their death. In addition to homework exercises for each chapter, the text contains a large number of questions that are meant to stimulate the understanding of the physical principles. Stellar evolution is the series of phases that a star. passes through between its birth and its death. The following article describes the evolution of typical stars. Formation The space between stars contains gas and dust at a very low density. The relevant physical processes, which include the equation of state, opacity, nuclear reactions and neutrino losses are then reviewed. Subsequent chapters describe the evolution of low-mass stars from formation to the final white dwarf phase. The final chapter deals with the evolution of massive stars. The primary factor determining how a star evolves is its mass as it reaches the main sequence. The following is a brief outline tracing the evolution of a low-mass and a high-mass star. The life of a star. Stars are born out of the gravitational collapse of cool, dense molecular clouds. As the cloud collapses, it fragments into smaller regions.
Intermediate-mass stars, between – M ☉ and 5–10 M ☉, pass through evolutionary stages similar to low mass stars, but after a relatively short period on the red giant branch they ignite helium without a flash and spend an extended period in the red clump before forming a degenerate carbon-oxygen core. Since their discovery, the W3, W4, and W5 regions have been extensively studied from multi-parsec down to AU size scales. W3 contains one of the richest and best studied populations of young, deeply embedded massive stars within 2 kpc of the Sun. W4 is one of the nearest examples of a galactic superbubble powered by the winds and supernovae of OB stars. In the outer layers of a low‐mass star, the dominant mode of energy transport becomes convective motion. The internal structures of high‐mass and low‐mass stars are thus essentially reversed from each other (see Figure 1). Figure 1; High‐mass versus low‐mass main sequence structure. A low-mass star uses hydrogen fuel so sluggishly that they can shine as main-sequence stars for billion to 1 trillion years — since the universe is only about billion years old.