Atoms, Stars, and Nebulae

In a nontechnical fashion, this book tells the story of how astronomy and physics work together to unravel many mysteries of stars and nebulae. Professor Aller's descriptions stress deeper understanding of these objects, not just a mere review of facts. After a succinct, nonmathematical excursion into the principles of radiation and atomic structure, he explains in simple terms the physical processes at work in stars and gaseous nebulae. A survey of masses, dimensions, luminosities, temperatures, and chemical compositions of stars is followed by an exploration of their interiors and how stars generate energy. The life histories of stars, from origin through final demise, sometimes through variability to beautiful nebulae, sometimes via violent explosions as supernovae, is recounted in detail. The exotic life histories of many double stars, some of which produce novae, are also described, and the origins of chemical elements in dense stellar cores and the vital role played by gas and dust between the stars is explained. The book closes with an account of the exciting new field of high-energy astronomy and the origin of cosmic rays. This is the ideal introduction to the important field of modern astrophysics for physics and astronomy students. It should also appeal to amateur astronomers interested in the life history of a star, be it a modest one such as our sun or a massive object destined to become a supernovae.

Science & Math

Aller, Lawrence H.

Astronomy & Space Science

Cambridge University Press

In a nontechnical fashion, this book tells the story of how astronomy and physics work together to unravel many mysteries of stars and nebulae. Professor Aller's descriptions stress deeper understanding of these objects, not just a mere review of facts. After a succinct, nonmathematical excursion into the principles of radiation and atomic structure, he explains in simple terms the physical processes at work in stars and gaseous nebulae. A survey of masses, dimensions, luminosities, temperatures, and chemical compositions of stars is followed by an exploration of their interiors and how stars generate energy. The life histories of stars, from origin through final demise, sometimes through variability to beautiful nebulae, sometimes via violent explosions as supernovae, is recounted in detail. The exotic life histories of many double stars, some of which produce novae, are also described, and the origins of chemical elements in dense stellar cores and the vital role played by gas and dust between the stars is explained. The book closes with an account of the exciting new field of high-energy astronomy and the origin of cosmic rays. This is the ideal introduction to the important field of modern astrophysics for physics and astronomy students. It should also appeal to amateur astronomers interested in the life history of a star, be it a modest one such as our sun or a massive object destined to become a supernovae.

This scarce antiquarian book is a facsimile reprint of the original. Due to its age, it may contain imperfections such as marks, notations, marginalia and flawed pages. Because we believe this work is culturally important, we have made it available as part of our commitment for protecting, preserving, and promoting the world's literature in affordable, high quality, modern editions that are true to the original work.

Atoms, Stars and Nebulae

Goldberg, Leo

Literature & Fiction

Kessinger Publishing

Astrophysics: Atmospheres of the Sun and Stars

The Ronald Press Company

This scarce antiquarian book is a facsimile reprint of the original. Due to its age, it may contain imperfections such as marks, notations, marginalia and flawed pages. Because we believe this work is culturally important, we have made it available as part of our commitment for protecting, preserving, and promoting the world's literature in affordable, high quality, modern editions that are true to the original work.

Atoms, Stars And Nebulae

Literary

This is a new release of the original 1945 edition.

Literary Licensing, LLC

Sects. 12, 13. 89 sequence and that subgiant and fainter stars in globular clusters have ultraviolet excesses. When dealing with stars whose physical properties are imperfectly under­ stood, such as in globular cluster stars, we cannot rely too heavily on the empiri­ cal calibration by the kinds of stars used to define Fig. 5, to determine their true, unreddened U-B, B-V curve. But if by a combination of arguments, principally the reddening in the region of the stars we do known about, we can assign a fairly probable unreddened U-B, B-V curve to a group of stars about which we know little, the argument may be turned around. In this case some information may be gained about the energy envelope of the stars by examining the differences between the normal two-color index curves for the unknown group of stars compared to the known. In general there seem to be two possible causes for different stars defining different normal sequences in the U-B, B-V plane. One, the relative energy distribution in the continuum in the U, B and V photometry bands are different. An example of this is the effect of the Balmer depression in supergiants. This, of course, requires deviation from black body radiation curves for one or both groups of stars. This cause seems to be the dominant effect for very blue, hot stars where the depression of the continuum by absorption lines is at a minimum.

Astrophysik II: Sternaufbau / Astrophysics II: Stellar Structure (Handbuch der Physik Encyclopedia of Physics, 11 / 51)

Payne-Gaposchkin, Cecilia

Wrubel, Marshal H.

Arp, H. C.

Burbidge, G. R.

Burbidge, E. Margaret

Suess, Hans E.

Urey, Harold C.

Ledoux, P.

Walraven, Th.

Deutsch, Armin J.

Schatzman, E.

Zwicky, F.

Springer

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